In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Information

● Facility Information Oral Session: International Conference Hall (Plaza Heisei 3F) Open 8:30 / Close 20:00 (Mon-Thu), 17:30 (Fri) Poster Session: Media Hall (Plaza Heisei 3F) and Multipurpose space (Plaza Heisei 1F) Open 8:30 / Close 20:00 (Mon-Thu), 17:30 (Fri)

● Conference Events Welcome Party: Main Foyer (3F) 18:15 – 20:00 (Mon) Poster Session: Media Hall (Plaza Heisei 3F) and Multipurpose space (Plaza Heisei 1F) Core time: 18:30 – 19:30 (Tue), 17:25 – 18:30 (Thu) Additional time: 19:00 – 20:00 (Wed), break time

-- Note: At the Tuesday poster session, a small amount of alcoholic beverage will be supplied. Optional Tour: pick-up at the main entrance of Plaza Heisei (1F) 13:00 – ~17:00 (Wed.) Banquet: Tokyo Conference Center Ariake 19:00 – 21:00 (Thu) *There are shuttle buses to the banquet place

● Tips - Registration Desk The desk is set at Main Foyer (Plaza Heisei 3F). Open 9:00 / Close 17:00 (Mon. – Thu.) *On-site payment will be available on Monday and Tuesday. - Wi-Fi Wi-Fi is available. SSID/PW will be posted in the conference place. - Maps/Access Rough maps are attached at the last page. Please refer our Lyot2019 website for more details.

1 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Conference Schedule * Invited Talk (bold): 40min (talk 30min + Q&A 10min). * Joint Talk (marked “(J)”): 25min (talk 20min for two + Q&A 5min). * Contributed Talk: 15min (talk 12min + Q&A 3min).

Monday (October 21) Time Name Title 9:00 Registration 10:00 Opening Exoplanet (Planet Population) 10:10 B. A. Biller Exoplanet Direct Imaging Surveys: the statistical picture 10:50 E. L. Nielsen The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10-100 AU 11:05 M. Ogihara Development of planet formation theory by comparison with observational data 11:45 Poster Pops 12:00 Lunch Instrument and Technology (Ground+) 13:30 D. Mawet High contrast imaging and spectroscopy of exoplanets deconstructed 14:10 N. Jovanovic First Light Results from the Keck Planet Imager and Characterizer 14:25 J. Pezzato Status of the Phase II design and development of the Keck Planet Imager and Characterizer 14:40 A. Vigan Bringing high-spectral resolution to VLT/SPHERE with a coupling to VLT/CRIRES+: status of the HiRISE project 14:55 Coffee break & Poster viewing 15:40 M. Langlois Status of the SPHERE/SHINE survey: From the observations to the exoplanet detection performances. 15:55 J. Lozi SCExAO: Current status and upgrades 16:10 T. Kotani Development of the Extremely High-Contrast, High Spectral Resolution Spectrometer REACH for the Subaru Telescope 16:25 K. L. Miller Spatial Linear Dark Field Control on SCExAO 16:40 B. Mazin Results from Microwave Kinetic Inductance Detectors for Exoplanet Direct Imaging 16:55 N. H. Fruitwala Active Speckle Control with Microwave Kinetic Inductance Detectors 17:10 B. L. Gerard Speckle Subtraction: Limitations and the Path Forward 17:25 C. Marois Imaging and Characterization of Rocky Earth-size Habitable Zone Planets in the Solar Neighborhood with TMT 17:40 Poster Pops 18:15 Welcome Reception

2 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Tuseday (October 22) Time Name Title 9:00 Announcement Disk Theory 9:10 R. Tazaki Effect of dust size and structure on scattered-light images of protoplanetary disks 9:25 M. Montesinos Radiative scale-height and shadows in protoplanetary disks 9:40 R. Dong Observing planet formation in protoplanetary disks 10:20 Coffee break & Poster viewing Disk Imaging 11:00 L. Perez Small-scale Substructures in Planet-forming Disks 11:40 M. Konishi Dust Filtration in T Tauri Star HP Cha 11:55 A. Bayo The illusive disk around TWA 7 12:10 Lunch 13:30 C. Ginski Optical and near-infrared scattered light imaging of protoplanetary disks 14:10 J. Hashimoto Near-infrared high resolution observations of protoplanetary disks with Subaru 14:50 Poster Pops 15:10 Coffee break & Poster viewing Instrument and Technology (Polarization) 16:00 F. Snik A polarized view of high-contrast imaging 16:40 R. van Holstein Polarization-dependent beam shifts upon metallic reflection in diffraction-limited astronomical telescopes and instruments 16:55 Short Break Combination 17:10 J. Birkby Revealing exoplanet atmospheres by combining high contrast imaging with high resolution spectroscopy 17:50 A. Zurlo The SPHERE view of our closest multi-planetary system: Proxima Centauri 18:05 T. D. Brandt Masses, Orbits, and New Planets and Brown Dwarfs from Combining Imaging with Astrometry and Radial Velocity 18:20 Poster Pops 18:30 Core Time Poster viewing session (with alcoholic beverage)

3 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Wednesday (October 23) Time Name Title 9:00 Announcement Exoplanet Imaging 9:10 Q. M. Konopacky Characterizing Directly Imaged Exoplanets 9:50 J. J. Wang Detailed Monitoring of the HR 8799 Planets 10:05 Coffee break & Poster viewing 10:40 K. K. Wilcomb Moderate Resolution Spectroscopy of Directly Imaged Exoplanets 10:55 N. Whiteford Directly-imaged atmospheric characterisation with TauREx retrievals 11:10 Poster Pops 11:30 Lunch

13:00 Excursion

19:00 Poster viewing

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Thursday (October 24) Time Name Title 9:00 Announcement Disk Imaging (Debris Disk) 9:10 M. A. MacGregor Using Debris Disks to Trace Planetary System Formation and Evolution 9:50 P. Kalas Debris disks imaged with the Gemini Planet Imager Exoplanet Survey 10:05 E. Choquet Analysis of the population of debris disks viewed with HST 10:20 K. A. Crotts A Deep Polarimetric Study of the Asymmetrical Debris Disk HD 106906 10:35 J. Milli The scattering phase function of debris disks 10:50 Coffee break & Poster viewing Observation/Data Reduction Techniques 11:30 M. Samland Exoplanet detection: A temporal approach for increasing contrast performance close to the inner working angle 11:45 F. Cantalloube Beyond Gaussianity for the speckle statistics, a new consensus for post-processing of high-contrast images. 12:00 R. Laugier Reconciling kernel-phase and coronagraphy: new steps towards combining the performance of opposing techniques. 12:15 Lunch Instrument and Technology (Coronagraph) 13:30 N. Murakami Photonics technology toward high-contrast imaging instruments 14:10 D. Doelman Overview and on-sky results of the vector-Apodizing Phase Plate coronagraph 14:25 E. Por The Phase-Apodized-Pupil Lyot Coronagraph (PAPLC): a simple, high-performance Lyot-style coronagraph with a small inner working angle 14:40 Coffee break & Poster viewing Future Plan and Facility (Ground) 15:20 J. K. Chilcote & Upgrading the Gemini planet imager: GPI 2.0 A. Boccaletti (J) SPHERE+, Reaching New Depths 15:45 H. Kawahara REACH: Scientific Overview of Extremely High-Contrast Spectroscopy at the Subaru Telescope 16:00 R. Jensen-Clem Exoplanet Imaging with the Planetary Systems Imager 16:15 G. Chauvin Planet formation and Exoplanets at the Era of the Extremely Large Telescope Exoplanet/disk Imaging & Future Plan and Facility (Space) 16:30 V. Bailey Overview of the WFIRST Coronagraph Instrument and exoplanet science 16:45 J. H. Debes Studying Disks at High Contrast with WFIRST/CGI 17:25 Poster viewing (Core time)

19:00 Banquet * We will arrange shuttle buses from the conference place to banquet place.

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Friday (October 25) Time Name Title 9:00 Announcement Exoplanet Imaging 9:10 K. B. Follette The Bright Future of Protoplanet Direct Imaging - Lessons Learned from the First Generation Magellan Giant Accreting Protoplanet Survey (GAPlanetS) 9:25 A. J. Bohn Young Suns Exoplanet Survey (YSES) reveals planets, brown dwarfs, and disks in Sco-Cen 9:40 T. O. B. Schmidt A tentative first direct detection of a circumplanetary disk 9:55 M. Kasper VISIR/NEAR, a 100-hour direct imaging search for low-mass planets in alpha Centauri 10:10 Coffee break & Poster viewing 11:00 T. Currie The Next Generation of Exoplanet Direct Imaging with Extreme Adaptive Optics 11:40 J. M. Stone Thermal-Infrared Integral Field Spectroscopy of Planets and Protoplanets 11:55 J. Leisenring Directly Imaging Exoplanets and Disks with JWST NIRCam 12:10 Lunch Instrument and Technology (Space) 13:30 G. Ruane The Decadal Survey Testbed: Demonstrating Technology for Imaging Earth-like Exoplanets with Future Space Telescopes 13:45 I. Laginja Laboratory demonstration of high contrast imaging on segmented apertures: Results from STScI HiCAT testbed 14:00 P. Willems NASA’s S5 Starshade Technology Development Activity 14:15 A. Harness Laboratory demonstration of 1e-10 contrast with a sub-scale starshade external occulter 14:30 Coffee break & Poster viewing Future Plan and Facility (Space) 15:15 C. Beichman Direct Imaging and Spectroscopy of Exoplanets with the James Webb Space Telescope 15:55 S. Hinkley High Contrast Imaging of Exoplanets and Exoplanetary Systems with JWST 16:35 L. A. Pueyo & Searching and characterizing exoplanetary gems with ECLIPS, the LUVOIR coronagraph instrument High Contrast Observations with the Habitable Exoplanet - Observatory (HabEx): Science Goals and B. Mennesson (J) Projected Capabilities

17:00 Concluding Remarks

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Poster Pops Schedule * Short talk: 1 min / poster

Date/Time Name Title Monday T. Uyama Characterizing a directly-imaged planet Kappa And b with SCExAO (Oct. 21) S. Itoh New Symmetrical Formulation of Hexagonally Segmented Telescopes B. Sutlieff A vector Apodising Phase Plate view of an exoplanet atmosphere 11:45-12:00 R. Belikov Theoretical Performance Limits for Coronagraphs on Obstructed and Unobstructed Apertures: How Much Can Current Designs be Improved? J. Kammerer Studying giant planet formation with Fourier plane imaging techniques J.H. Girard The 2019 WFIRST Exoplanet Imaging Data Challenge S.C. Eriksson Near-visual integral-field spectroscopy of the circumbinary planet / brown dwarf 2M0103(AB)b with the new Narrow Field Mode on MUSE. Monday R. Morgan A Standard comparison of exoplanet yield for the LUVOIR and HabEx (Oct. 21) Concept Studies. S. P. Bos Focal-plane wavefront sensing with the vAPP: on-sky demonstration at SCExAO 17:40-17:50 N. I. Godoy Barraza New algorithms to improve the quality of NACO coronagraphic images. J. Zhang New NIR Polarimetric Differential Imaging Modes on the Subaru Coronagraphic Extreme Adaptive Optics Instrument T. Currie Developing and Demonstrating Linear Dark Field Control for Exo-Earth Imaging with the Ames Coronagraph Experiment Testbed C. Mejia Prada Deformable Mirrors Controller Architectures for High-Contrast Imaging Overview Tuesday T. Stolker MIRACLES: an atmospheric characterization survey of planetary and (Oct.22) substellar companions at 4-5 micron R.T. Tominaga Formation of axisymmetric substructures via secular instabilities triggered 14:50-15:10 by dust-gas friction and turbulent viscosity in protoplanetary disks S.Z. Takahashi Structure of the protoplanetary disk around V1094 Sco obtained from dust continuum emission and SED D. Tamayo Detecting distant, sub-Jovian planets in scattered light through their circumplanetary debris disks S. Mayama ALMA reveals a misaligned, HCO+-rich, inner gas disk inside the large cavity of the transitional disk around J160421.7-213028 G.M. Strampelli Unveiling a population of substellar binary companions in a young cluster: HST survey of the Orion Nebula Cluster in the H2O 1.4 µm absorption band J. Hom Comparison of PSF Subtraction Algorithms on Disk Imaging Data D.M. van Dam High Resolution Polarisation Imaging of 1SWASP J140747.93-394542.6 The Search for an Extrasolar Ring System J. Gonzalez-Quiles WFIRST Coronagraph Exoplanet Scene Simulations W.R. Thompson Searching for Additional Outer Planets Around HR8799 N. Engler The VIBES Exoplanet Survey with SPHERE N. Engler SPHERE Observations of Debris Disks Tuesday (Oct. 22)

18:20-18:30

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Wednesday A. Boehle Combining high contrast imaging and radial velocities to constrain the (Oct. 23) planetary architecture of nearby stars

11:10-11:30 T. Groff The Parabolic Deformable Mirror Testbed at Goddard Space Flight Center A.J. Riggs Results with FALCO, a Software Package for Coronagraphic Wavefront Correction A. Takahashi Laboratory demonstration of a cryogenic deformable mirror for wavefront correction of space-borne infrared telescopes A. Vigan On-sky validation of the ZELDA wavefront sensor for the calibration of non-common path aberrations in VLT/SPHERE A. Vigan First constraints on the population of young giant exoplanets from the SPHERE infrared survey for exoplanets (SHINE) R. Nakatani Radiation Hydrodynamics Simulations of Photoevaporating Protoplanetary Disks with Various Metallicities G. Otten Performance simulations of the high-res characterization of directly imaged planets with HiRISE G. Aerna SPHERE reveals warped disk around HD 139614 F. Martinache Robust high contrast imaging with kernel-nulling interferometry

8 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Poster Titles

Exoplanet Imaging No. Name Title P1-01 T. Uyama Characterizing a directly-imaged planet Kappa And b with SCExAO P1-02 J. K. Ward Duong Gemini Planet Imager Spectroscopy of the Reddest Known Substellar Companion HD206893 B P1-03 P. Calissendorff Spectral characterization of newly detected young substellar binaries with SINFONI P1-04 A. Vigan First constraints on the population of young giant exoplanets from the SPHERE infrared survey for exoplanets (SHINE) P1-05 N. Engler The VIBES Exoplanet Survey with SPHERE P1-06 M. Janson BEAST: The B-star Exoplanet Abundance Study P1-08 D. M. van Dam High Resolution Polarisation Imaging of 1SWASP J140747.93-394542.6 The Search for an Extrasolar Ring System P1-09 J. H. Girard Imaging gap-carving, accreting protoplanets with MUSE P1-10 S. C. Eriksson Near-visual integral-field spectroscopy of the circumbinary planet / brown dwarf 2M0103(AB)b with the new Narrow Field Mode on MUSE. P1-11 M. Bonnefoy Planets and protoplanets revealed by the molecular mapping technique. P1-12 T. Stolker MIRACLES: an atmospheric characterization survey of planetary and substellar companions at 4-5 micron P1-13 W. R. Thompson Searching for Additional Outer Planets Around HR8799 P1-14 M. L. Bryan First Constraints on the 3D Angular Momentum Architecture of a Planetary System P1-15 G. M. Strampelli Unveiling a population of sub-stellar binary companions in a young cluster: HST survey of the Orion Nebula Cluster in the H2O 1.4 µm absorption band P1-16 C. Fontanive The new COPAINS tool for target selection and orbital characterisation of direct imaging systems P1-17 D. Tamayo Detecting distant, sub-Jovian planets in scattered light through their circumplanetary debris disks P1-18 A. Skemer Imaging Temperate Exoplanets P1-19 Z. Briesemeister High Spatial Resolution Thermal Infrared Integral Field Spectroscopy P1-20 G. Singh Active minimization of non-common path aberrations using a self-coherent camera for imaging exoplanetary systems. P1-21 C. Dahlqvist RSM detection map for direct exoplanet detection in ADI sequences P1-22 E. Bendek Deformable Mirrors Controller Architectures for High-Contrast Imaging Overview P1-23 L. Y. C. Leboulleux How to speed up your simulations of ground-based images P1-24 J. H. Girard Generating Realistic Coronagraphic Images of Point Source Detections with JWST's NIRCam and MIRI P1-25 J. Llop Sayson Searching for Alpha Centauri A Companions with the James Webb Space Telescope MIRI Coronagraphic Mode P1-26 C. Mejia Prada The WFIRST Coronagraph telescope simulator: Building a coronagraph calibrator P1-27 J. Gonzalez-Quiles WFIRST Coronagraph Exoplanet Scene Simulations

Exoplanet Theory No. Name Title P2-01 Y. Aoyama Theoretical modeling of Hα spectral profile with 1D-radiation-hydrodynamic simulation: constraining the accretion rate and mass of the protoplanets PDS70b and c P2-02 S. WANG Formation of Planetary Systems in Mean Motion Resonances 9 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Disk Imaging Name Title P3-01 M. Honda Water ice mapping toward protoplanetary disk P3-02 Y. Yang Subaru Telescope High-contrast Observations of disks in multiple systems P3-03 S. Jin New constraints on the dust and gas distribution in the LkCa 15 disk P3-04 S. Z. Takahashi Structure of the protoplanetary disk around V1094 Sco obtained from dust continuum emission and SED P3-05 M. Momose Investigating the gas-to-dust ratio in the protoplanetary disk of HD 142527 P3-06 S. Mayama ALMA reveals a misaligned, HCO+-rich, inner gas disk inside the large cavity of the transitional disk around J160421.7-213028 P3-07 S. Kim The derivation of the dust properties using the synthetic ALMA multiband analysis P3-08 S. Kim The detection of a dust ring beyond the outer edge of the dust disk around CR Cha P3-09 G. Singh Discovery of an azimuthal density gradient in a gas-rich debris disk possibly related to a massive collision P3-10 C. Perrot First resolved observations of a highly asymmetric debris disc around HD 160305 with VLT/SPHERE P3-11 C. Perrot First detection of a very sharp ring in near-infrared light with VLT/SPHERE around HD 121617. P3-12 N. Engler SPHERE Observations of Debris Disks P3-13 J. Olofsson Dust production in young debris disks P3-14 J. Mazoyer The Surprising Scattering Phase Function of HR 4796 A P3-15 S. G. Wolff HD 146897; An Icy Debris Disk as seen by the Gemini Planet Imager P3-16 J. Patience A Survey for Resolved Debris Disks in the Sco-Cen Association P3-17 J. Hom Comparison of PSF Subtraction Algorithms on Disk Imaging Data P3-18 C. A. Grady The Eroding Disk of AU Mic: Implications for the Habitability of M-star Terrestrial Planets P3-19 P. Hinz The Hunt for Observable Signatures of Terrestrial planetary Systems (HOSTS): How Much Dust should We Expect in the Habitable Zone? P3-20 E. S. Douglas A high-contrast SmallSat Mission Concept P3-21 G. M. Aerna SPHERE reveals warped disk around HD 139614

Disk Theory No. Name Title P4-01 R. T. Tominaga Formation of axisymmetric substructures via secular instabilities triggered by dust-gas friction and turbulent viscosity in protoplanetary disks P4-02 Y. Sakurai Clustering and collision statistics of dust particles in weakly compressible turbulence in protoplanetary disks P4-03 M. Kunitomo Dispersal of Protoplanetary Disks with Magnetically-driven and Photoevaporative Winds P4-04 R. Nakatani Radiation Hydrodynamics Simulations of Photoevaporating Protoplanetary Disks with Various Metallicities

Instrument and Technology No. Name Title P5-01 F. Cantalloube SPHERE: the current contrast limitations

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P5-02 O. Guyon Prototyping High Contrast Imaging for ELTs on SCExAO: Users’ Guide and Recent Highlights P5-03 J. Zhang New NIR Polarimetric Differential Imaging Modes on the Subaru Coronagraphic Extreme Adaptive Optics Instrument P5-04 A. Sahoo Astrometry and Photometry with Satellite Speckles P5-05 D. Vassallo Overview of the coronagraphic capabilities of SHARK-NIR, the second- generation high contrast imager for the Large Binocular Telescope P5-06 E. Carolo XAO-assisted coronagraphy with SHARK-NIR: from simulations to laboratory tests P5-07 S. Itoh New Symmetrical Formulation of Hexagonally Segmented Telescopes P5-08 R. Galicher Wrapped Vortex: a Cheap Achromatic Coronagraph Phase Mask P5-09 D. Rouan Continuous phase mask “à la four-quadrant” optimized for achromatism and bandpass. P5-10 J. Nishikawa Combination of apodized pupil and phase mask coronagraph for Subaru Telescope P5-11 J. Lozi Polychromatic analysis of the coronagraphs in SCExAO P5-12 C. Lopez Chromatic Performance Of A Vector Vortex Coronagraph P5-13 J. G. Kuhn SLM-based Digital Adaptive Coronagraphy: Status, performance update, and future prospects P5-14 K. Fogarty Towards High Throughput and Low-Order Aberration Robustness for Vortex Coronagraphs with Central Obstructions P5-15 K. Enya Heritage of technology for mid-infrared coronagraph onboard space-borne telescopes for exoplanet characterization P5-16 M. N'Diaye Imaging short orbit exoplanets from the ground with novel Apodized Pupil Lyot Coronagraphs P5-17 T. Currie Developing and Demonstrating Linear Dark Field Control for Exo-Earth Imaging with the Ames Coronagraph Experiment Testbed P5-18 R. Belikov Theoretical Performance Limits for Coronagraphs on Obstructed and Unobstructed Apertures: How Much Can Current Designs be Improved? P5-19 R. Juanola- Sensitivity to telescope aberrations for exoplanet detection with the Parramon LUVOIR coronagraph instrument ECLIPS P5-20 S. Hildebrandt SISTER: Simulating Exoplanetary Systems as observed with Starshade P5-21 A. Vigan On-sky validation of the ZELDA wavefront sensor for the calibration of non-common path aberrations in VLT/SPHERE P5-22 S. P. Bos Focal-plane wavefront sensing with the vAPP: on-sky demonstration at SCExAO P5-23 S. B. Vievard Overview of focal plane wavefront sensors to correct for the Low Wind Effect on SUBARU/SCExAO P5-24 M. Langlois Mach-Zehnder Wavefront sensor for XAO: From laboratory tests to on sky measurements using the SCAO capability of CANARY at the William Hershel Telescope P5-25 G. W. Allan Deep Neural Networks Improve the Dynamic Range of Lyot-based Low Order Wavefront Sensing P5-26 A. Takahashi Laboratory demonstration of a cryogenic deformable mirror for wavefront correction of space-borne infrared telescopes P5-27 A. J. E. Riggs Results with FALCO, a Software Package for Coronagraphic Wavefront Correction P5-28 E. Cady Wavefront control and calibration for the WFIRST Coronagraph Instrument P5-29 D. Sirbu Applications of Multi-Star Wavefront Control to WFIRST, HABEX, and LUVOIR P5-30 M. Perrin Wavefront Control and Modeling for High Contrast on Segmented Apertures: Results from the HiCAT Testbed P5-31 A. Potier Comparing Focal Plane Wavefront Sensors on THD2 bench : Self-coherent camera, Pair Wise Probing and COFFEE P5-32 P. Baudoz Overview of the THD2 performance

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P5-33 T. Groff The Parabolic Deformable Mirror Testbed at Goddard Space Flight Center P5-34 R. E. Morgan Assembly, Integration, and Testing of the Deformable Mirror Demonstration Mission (DeMi) CubeSat Payload P5-35 J. Llop Sayson New high contrast technology demonstrations at the High-Contrast Spectroscopy Testbed for Segmented Telescopes (HCST) P5-36 G. Otten Performance simulations of the high-res characterization of directly imaged planets with HiRISE P5-37 C. Beichman The Promise of Diffraction Limited Spectrometers for Exoplanet Characterization P5-38 C. Coker Progress Towards a Laboratory Demonstration of a Multi-Object, Single- Mode Fiber Spectrograph P5-39 E. Huby Spectroscopy below the diffraction limit with FIRSTv2 at the Subaru Telescope P5-40 R. D. Stelter An Introduction to SCALES, the Next-Generation Exoplanet Spectrograph P5-41 G. MORETTO Partially Filled Aperture Interferometric Telescopes Achieving Large Aperture and Coronagraphic Performance — The Exo-Life Finder (ELF) Telescope. P5-42 D. Echeverri Vortex Fiber Nulling for Exoplanet Observations: Concept, Laboratory Results, and Planned On-Sky Deployment P5-43 E. Serabyn Detecting companions inside the coronagraphic regime with nulling interferometry P5-44 F. Martinache Robust high contrast imaging with kernel-nulling interferometry P5-45 E. Maier Implementing Multi-wavelength Fringe Tracking for the LBTI's Phase Sensor, PHASECam P5-46 K. H. Yip Pushing the Limits of Exoplanet Discovery via Direct Imaging with Deep Learning

Observation/Data Reduction Techniques No. Name Title P6-01 M. Perrin Data Processing and Calibrations for the Gemini Planet Imager Exoplanet Survey P6-02 R. van Holstein A highly-automated end-to-end pipeline to reduce VLT/SPHERE-IRDIS polarimetric data P6-03 A.-M. LAGRANGE Comparison between SPHERE and GPI astrometries P6-04 G. Zhao High-contrast Imaging technique combining IRS and ADI P6-05 N. I. Godoy Barraza New algorithms to improve the quality of NACO coronagraphic images. P6-06 J. Kammerer Studying giant planet formation with Fourier plane imaging techniques P6-07 Y. Xin Numerical Investigations of Coronagraphic Self-Calibration P6-08 P. Patapis Exploring the limits of directly imaging exoplanets with the Medium Resolution Imaging Spectrograph on JWST MIRI P6-09 B. Sutlieff A vector Apodising Phase Plate view of an exoplanet atmosphere P6-10 I. Waldmann Atmospheric retrievals of directly imaged planets using TauREx3 and deep learning P6-11 N. Nikolaou Refining exoplanet atmospheric retrievals with information-theoretic methods

Combination No. Name Title P7-01 A. Boehle Combining high contrast imaging and radial velocities to constrain the planetary architecture of nearby stars P7-02 M. Kenworthy Results from the Beta Pictoris b Hill Sphere Transit Campaign P7-03 D. Savransky Looking for Planets in all the Right Places: Target Selection for Direct Imaging P7-04 J. H. Girard The 2019 WFIRST Exoplanet Imaging Data Challenge

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Future Plan and Facility No. Name Title P8-01 M. Fitzgerald An Overview of the TMT Planetary Systems Imager P8-02 O. Absil The game-changing promises of ELT/METIS for exoplanet imaging P8-03 M. Houlle Exoplanet direct detection and characterization with the ELT/HARMONI integral field spectrograph P8-04 R. Hu Exoplanet Sciences with Starshade P8-05 R. Morgan A Standard comparison of exoplanet yield for the LUVOIR and HabEx Concept Studies P8-06 K. Stapelfeldt The NASA/NSF Extreme Precision Radial Velocity Initiative P8-07 K. Stapelfeldt The NASA Exoplanet Exploration Program Science Gap List

Others No. Name Title P9-01 M. Ban Chasing free-floating planet from a parallax observation of a microlensing event P9-02 T.-S. Pyo High contrast shock emission structures around VV CrA in datacube data achieved by high spectral resolution (R ~45000) P9-03 K. Takizawa Vegetation red edge on water planets around M-dwarfs

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Talk Abstract

No. Title Abstract Time Name (Affiliation) O-01I Exoplanet Direct Large scale direct imaging exoplanet surveys yield three key scientific outputs: 1) new Imaging Surveys: the discoveries, 2) characterisation of known objects, and 3) statistical constraints on the underlying statistical picture exoplanet population. Multiple 400-600 star surveys with 8-m class telescopes and extreme AO 10/21 coronagraphs, such as SPHERE SHINE and Gemini GPIES, are nearing their end, as well as Mon. smaller targeted surveys to determine exoplanet frequency around samples such as binary stars. 10:10- Beth Alison Biller I will briefly summarise detections from these surveys, and focus in detail on what we have (University of learned about the statistical distribution of young giant planets, including observed trends with Edinburgh) host star mass and differences between exoplanet and brown dwarf populations. I will discuss comparisons to both empirical distributions and simulated populations from disk instability and core accretion models. O-02 The Gemini Planet The Gemini Planet Imager Exoplanet Survey (GPIES) has observed 521 young, nearby stars, Imager Exoplanet making it one of the largest, deepest direct imaging surveys for giant planets ever conducted. Survey: Giant Planet With detections of six planets and four brown dwarfs, including the new discoveries of 51 10/21 and Brown Dwarf Eridani b and HR 2562 B, GPIES also has a significantly higher planet detection rate than any Mon. Demographics from 10- published imaging survey. Our analysis of the uniform sample of the first 300 stars reveals new 10:50- 100 AU properties of giant planets (>2 MJup) from 3-100 AU. We find at >3 sigma confidence that these planets are more common around high-mass stars (>1.5 solar masses) than lower-mass stars. We also present evidence that giant planets and brown dwarfs obey different mass Eric L. Nielsen functions and semi-major axis distributions. Our direct imaging data imply that the giant planet (KIPAC/Stanford) occurrence rate declines with semi-major axis beyond 10 AU, a trend opposite to that found by radial velocity surveys inside of 10 AU; taken together, the giant planet occurrence rate appears to peak at 3-10 AU. All of these trends point to wide-separation giant planets forming by core/pebble accretion, and brown dwarfs forming by gravitational instability. O-03I Development of planet After the discovery of the first exoplanet, there has been spectacular progress in the observation formation theory by of exoplanets. Thanks to this, planet formation theory has also been significantly improved. For comparison with example, it is pointed out that the density distribution of a protoplanetary disk can be different 10/21 observational data from the classical disk model with a simple power-law distribution. The change in the disk Mon. model modifies the picture of orbital migration. In addition, in the recent planet formation 11:05- model, effects of a pebble accretion in which planets grow by accreting small particles are Masahiro Ogihara intensely investigated. In this presentation, we will discuss the current planet formation theory (National Astronomical by comparing results of planet formation simulation with observational findings. A large Observatory of Japan) number of super-Earths have been discovered in close-in orbits, which helped to improve planet formation theory. For example, it has been revealed that close-in super-Earths would form through orbital instability of a chain of resonant planets. On the other hand, as the number of observed wide-orbit planets is limited, formation models of such planets are not well established. To develop a robust planet formation theory, observational data of wide-orbit planets are awaited. O-04I High contrast imaging Exoplanet science has revolutionized our view of the Universe and ushered in the second and spectroscopy of Copernican revolution. After nearly three decades of exoplanet hunting, we now know of more exoplanets than 4000 confirmed exoplanets. The Solar system, the only planetary system we had ever 10/21 deconstructed contemplated until the 1990s, is now one example amongst a mind-boggling variety of system Mon. architectures. So far, the vast majority of these planetary systems have been discovered 13:30- indirectly by the radial velocity, transit, or microlensing techniques. All three methods have Dimitri Mawet limited remote sensing capabilities. Apart from inferred bulk compositions, we do not know (Caltech) much about these exoplanets and their atmospheres. Select transiting and close-in systems are amenable to spectroscopic analysis, which can determine the molecular composition of the upper layers of planetary atmospheres, but remain hampered by prevalent clouds and hazes. Beyond taking striking pictures, high contrast imaging promises to yield the most detailed measurements of distant planetary systems, from atmospheric composition and dynamics to orbital configurations and planet disk interactions. Separating the signal of a faint exoplanet orbiting its host star has been a significant technical challenge and has thus far limited us to the study of long-period relatively bright young giant exoplanets. Future ground-based and space- based giant telescopes will be pushing down to the regime of temperate Earth-size exoplanets, which present a quantum leap in contrast and inner working angle capabilities. Along the way, direct detection and characterization will shed invaluable light on a wide range of planet types,

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including mini-Neptunes and super-Earths. In this talk, I will provide a short tutorial on current techniques and review technology developments involving laboratory and on-sky proof-of- concepts that aim at bridging this gap and help realize the full potential of high contrast imaging and spectroscopy. O-05 First Light Results High-resolution spectroscopy will enable detailed characterization of the composition and from the Keck Planet dynamics of exoplanets through measurements of individual spectral lines. The Keck Planet Imager and Imager and Characterizer (KPIC) consists of upgrades to the Keck II adaptive optics (AO) 10/21 Characterizer system and instrument suite. This presentation will provide an overview of the new capabilities Mon. KPIC brings to the WM Keck Observatory as well as highlight the first light science results 14:10- from the novel infrared pyramid wavefront sensor (PyWFS) and the fiber injection unit (FIU) of Nemanja Jovanovic KPIC. (Caltech) The PyWFS provides high performance wavefront correction on red objects allowing for detailed imaging when combined with NIRC2 and spectroscopic characterization when the FIU is used to isolate and inject the planet light from the AO system into the NIRSPEC spectrograph via a single mode fiber. By combining high-contrast imaging and high-resolution spectroscopy, the KPIC FIU is the first instrument to implement high dispersion coronagraphy to study faint imaged exoplanets close to their host stars at high spectral resolution. We are obtaining K-band R~35,000 exoplanet spectra sensitive to spectral lines of water, methane, and carbon monoxide in their atmospheres, as well as planetary radial velocities and spin rates. These measurements provide insights into the composition, formation, and accretion history of these young gas giants. I will provide an overview of the capabilities of KPIC and early science results from data we have obtained this year. O-06 Status of the Phase II The Keck Planet Imager and Characterizer comprises of a series of upgrades to the Keck II design and adaptive optics system to improve the direct imaging and high resolution spectroscopy development of the capabilities of the facility instruments NIRC2 and NIRSPEC, respectively. Phase I of KPIC 10/21 Keck Planet Imager includes a NIR pyramid wavefront sensor and Fiber Injection Unit (FIU) to feed NIRSPEC with Mon. and Characterizer a single mode fiber, which have already been installed and are currently undergoing 14:25- commissioning. KPIC will enable High Dispersion Coronagraphy (HDC) of directly imaged exoplanets for the first time, providing high-contrast high-resolution spectroscopic data for the Jacklyn Pezzato characterization of exoplanet atmospheres (Doppler imaging, spin measurements, and molecular (California Institute of detection and mapping). This science goal drives the development of Phase II of KPIC, which is Technology) scheduled to be deployed in early 2020. Phase II optimizes the system throughput and starlight suppression using a variety of additional submodules, including a 952-element deformable mirror, phase induced amplitude apodization lenses, an atmospheric dispersion compensator, multiple coronagraphs, a Zernike wavefront sensor, and multiple science ports. All sub-modules are geared to the tasks of maximizing throughput and/or improving raw contrast, hence reducing integration time by a factor of 100 and allowing the characterization of close exoplanets that are not currently accessible to any other instrument. A testbed is being built in the Exoplanet Technology Lab at Caltech to characterize and test the design of each of these submodules before KPIC Phase II is deployed to Keck. We present an overview of the design of Phase II and report on results from laboratory testing. O-07 Bringing high-spectral New generation exoplanet imagers on large ground-based telescopes are highly optimized for resolution to the detection of young giant exoplanets in the near-infrared, but they are intrinsically limited for VLT/SPHERE with a their characterization by the low spectral resolution of their integral field spectrographs 10/21 coupling to (R<100). High-dispersion spectroscopy at R=105 would be a powerful tool for the Mon. VLT/CRIRES+: status characterization of these planets, but there is currently no high-resolution spectrograph with 14:40- of the HiRISE project extreme adaptive optics and coronagraphy that would enable such characterization. With project HiRISE we propose to use near-infrared fiber coupling to combine the capabilities of two flagship instruments at the Very Large Telescope in Chile: the high-contrast exoplanet imager Arthur Vigan SPHERE and the high-resolution spectrograph CRIRES+. This coupling will enable detailed (Laboratoire characterization of directly-imaged exoplanets and open new possibilities such as measuring d'Astrophysique de their orbital and rotational velocity or attempting the detection of yet unseen exoplanets. In this Marseille / CNRS) presentation, we will provide a general overview of the project status. We will first detail the design of the coupling, based on the implementation of a fiber injection module in SPHERE, a 55 meter fiber bundle around the telescope and a fiber extraction module in CRIRES+. Then we will present our strategy for the planet acquisition, supported by laboratory demonstrations on our MITHiC high-contrast imaging testbed. And finally we will conclude with the the foreseen implementation plan at the telescope.

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O-08 Status of the With the development of high contrast imaging techniques and instruments, vast efforts have SPHERE/SHINE been devoted during the past decades to detect and characterize lighter, cooler and closer survey: From the companions to nearby stars, and ultimately image new planetary systems. Complementary to 10/21 observations to the other planet-hunting techniques, this approach has opened a new astrophysical window to study Mon. exoplanet detection the physical properties and the formation mechanisms of brown dwarfs and planets. The SHINE 15:40- performances. survey for SPHERE High-contrast ImagiNg survey for Exoplanets, is a large direct imaging near-infrared survey of 600 young, nearby stars carried out in the context of the SPHERE consortium Guaranteed Time Observations representing 200 nights spread between 2015 and Maud Langlois 2020. Our scientific goals are to characterize known planetary systems (architecture, orbit, (CNRS/CRAL) stability, luminosity, atmosphere), to search for new planetary systems using SPHERE’s unprecedented performances, finally to determine the occurrence and orbital and mass function properties of the wide orbit, giant planet population as a function of the stellar host mass and age. In this talk, we will briefly present the main properties of the SHINE sample, the observing and data reduction and analysis strategy, the current detection performances achieved with the combination of both near-infrared instruments IRDIS and IFS, finally the key early results obtained so far with the characterization of giant planets, the study of planetary system architectures. O-09 SCExAO: Current The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument is a high-contrast status and upgrades imager installed at the 8-m Subaru Telescope on Maunakea, Hawaii. SCExAO is both an instrument open for use by the international scientific community, and a testbed validating new 10/21 technologies that are critical to future high-contrast imagers on Giant Segmented Mirror Mon. Julien Lozi Telescopes (GSMTs). Since its first light, SCExAO has grown in capabilities and complexity to 15:55- (NAOJ - Subaru integrate the most advanced technologies available today in detectors, wavefront sensors, real- Telescope) time control, and starlight suppression. Its modular design allows for collaborators to implement their own hardware and algorithms, and to test them on-site or remotely. We are now commissioning the Microwave Kinetic Inductance Detector (MKID) Exoplanet Camera (MEC) for high-speed speckle control, as well as high frame rate low noise NIR detectors such as the Leonardo SAPHIRA detector. A New Spectropolarimetric mode using CHARIS was recently deployed. New coronagraphic modes include the Phase Induced Amplitude Apodization Complex Mask Coronagraph (PIAACMC), or the vector Apodizing Phase Plate (vAPP) coronagraph. Innovative wavefront control algorithms are also being tested, such as predictive control, multi-camera machine learning sensor fusion, and focal plane wavefront control. We present here the current status of the SCExAO instrument, with an emphasis on collaborations and recent technology demonstrations, as well as the upgrades planned for the near future. O-10 Development of the Detection of molecular species in exoplanetary atmospheres is fundamental to their Extremely High- characterization. Of particular interest to the search for habitable exoplanets are, the detection of Contrast, High Spectral water and oxygen in their atmospheres; obtaining these measurements is regarded as the next 10/21 Resolution breakthrough in the search for life on other planets. One promising method is a combination of Mon. Spectrometer REACH an Extreme AO, coronagraphs and a single-mode fiber fed, NIR high-dispersion spectrograph. 16:10- for the Subaru The ExAO+coronagraph can significantly reduce the scattered light from a central star and Telescope inject planet light into the high-dispersion spectrograph with high efficiency, which can directly detect the pattern of the molecular lines through cross-correlation analysis. REACH (Rigorous Exoplanetary Atmosphere Characterization with High dispersion Takayuki Kotani coronography) is an instrument to realize very high spectral resolution, over R>100,000 at (Astrobiology center/ extreme contrast by combining the high-resolution spectrograph InfraRed Doppler (IRD) and NAOJ) the extreme adaptive optics instrument, SCExAO at the Subaru Telescope. REACH consists of mini-IFU like 7 single-mode fiber bundle located at a focus of SCExAO, a high-speed photometric monitoring camera for the output beams from the fiber bundle, and a beam switching and feed system from the fiber bundle to IRD’s 2 single-mode fibers. REACH can collect planetary spectra contemporaneously with that of the primary star, which allows precise telluric removal, especially important in the NIR wavelengths. Thanks to the mode-filtering capability of a single-mode fiber, speckle light injected into a fiber will be reduced by at least 2 orders of magnitude compared to the multi-mode fiber injection of IRD. A photometric monitoring module, which images the light not used by IRD will be used for real-time speckle nulling and fiber injection optimization, which can further reduce the speckle light injected into fibers. We will provide an overview of the instrument and present the results from on-sky tests scheduled in October. We will also discuss the future prospects of combining extremely high- contrast and high-spectral resolution methods leading to an exoplanet instrument for the TMT/E-ELT.

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O-11 Spatial Linear Dark One of the key challenges facing direct exoplanet imaging is the continuous maintenance of the Field Control on region of high contrast within which light from the exoplanet can be detected above the stellar SCExAO noise. In high-contrast imaging systems, one of the dominant sources of aberration is the 10/21 residual wavefront error (WFE) that arises due to non-common path aberrations (NCPA). Slow Mon. variations in the NCPA generate quasi-static speckles in the image plane, post-AO correction, 16:25- Kelsey Lynn Miller which degrade the dark hole contrast. On the Subaru Coronagraphic Extreme Adaptive Optics (Leiden Observatory, instrument (SCExAO), one of the coronagraphic modes is a vector apodizing phase plate Leiden University) (vAPP) which generates two 180 degree dark holes with approximately 10-4 contrast at lambda = 1550 nm. In this system, the residual WFE due to NCPA is less than 100 nm. In this paper, we present a method with which to sense time-varying NCPA, thereby suppressing the resultant quasi-static speckles within the dark hole. This algorithm, referred to as spatial linear dark field control (LDFC), is a focal plane wavefront sensing technique which measures variations in intensity in the bright field opposite the dark hole to sense small aberrations that modify both the bright field and the dark hole. Spatial LDFC is a linear operation and does not require deformable mirror (DM) modulation, therefore allowing it to run fast enough to address not just quasi-static NCPA, but also faster-moving atmospheric turbulence residuals. Here we present simulations of spatial LDFC's expected performance on SCExAO as well as preliminary results of the algorithm deployed at Subaru Telescope using the compute and control for adaptive optics (cacao) open source package to control quasi-static NCPA. The results shown here demonstrate the ability of spatial LDFC to improve SCExAO's high-contrast imaging capabilities for direct exoplanet imaging. Next steps include increasing the speed to address not only NCPA but also faster moving chromatic terms in residual atmospheric turbulence. Use of the open source cacao package will also allow for easy deployment of this algorithm on other systems such as MagAO-X on the Magellan Clay Telescope and the Keck Planet Imager and Characterizer (KPIC) on the Keck Telescope. On-sky results at Subaru are expected by early 2020. O-12 Results from Microwave Kinetic Inductance Detectors, or MKIDs, are superconducting detectors that can Microwave Kinetic serve as noise-free integral field spectrographs on a chip in the optical and near-IR. Our lab has Inductance Detectors built and been operating two instruments based on MKIDs, the 10 kpix DARKNESS instrument 10/21 for Exoplanet Direct at the Palomar Hale Telescope which works with P3K and SDC, and the 20 kpix MEC at the Mon. Imaging Subaru Telescope mounted to SCExAO. Here I will review the performance of the instruments 16:40- and describe a powerful new technique using individual photon arrival times for speckle discrimination. This new technique allows us to dig below the classical photon noise limit Ben Mazin derived from perfect subtraction of the static PSF with techniques like ADI and SDI, and is (University of California effective even at small inner working angles. I will also show the first scientific results from Santa Barbara) MEC, the MKID exoplanet camera on Subaru SCExAO.

O-13 Active Speckle Control We present the development and testing of focal plane wavefront control techniques that utilize with Microwave Microwave Kinetic Inductance detectors (MKIDs) as a focal plane IFU. MKIDs are ideally Kinetic Inductance suited to this application, as they are energy resolving, and have single photon sensitivity, zero 10/21 Detectors read noise, and microsecond time resolution. These characteristics enable much higher feedback Mon. rates than conventional systems; for the first time, focal plane science camera measurements 16:55- may be used to correct atmospheric aberrations in addition to quasistatics. We have developed Neelay Hitesh Fruitwala speckle nulling code for MEC, a 20,000 pixel IFU behind SCExAO at Subaru Observatory. Our (University of California code is optimized for fast operation in the low signal-to-noise regime, and uses the CACAO at Santa Barbara) image format for low-latency communication with the main AO control loop. We will present preliminary results from laboratory testing, including achievable contrast/speckle noise floor and loop convergence times in a variety of conditions (quasistatic and simulated turbulence). O-14 Speckle Subtraction: Direct detection and detailed characterization of exoplanets using extreme adaptive optics Limitations and the (ExAO) is a key science goal of both current and future extremely large telescopes. However, Path Forward both chromatic and temporal wavefront errors currently limit the sensitivity of this endeavor. 10/21 I will first demonstrate the effect of these limitations using on-sky datasets taken with the Mon. Subaru Coronagraphic ExAO system. I will then illustrate a path forward: fast focal plane 17:10 Benjamin L. Gerard wavefront sensing of both quasi-static and residual atmospheric speckles. Our new method, (University of Victoria) called the Fast Atmospheric Self-coherent camera Technique (FAST), is designed precisely to overcome these limitations. I will present FAST results from both numerical simulations and laboratory testing and discuss ongoing plans for on-sky implementation. Looking toward the future, the sensitivity improvement from focal plane wavefront sensing techniques such as FAST will play an essential role in the ground-based detection and characterization of lower mass and/or colder exoplanets.

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O-15 Imaging and TMT, with an impressive ~200x gain (D4) in integration time compared to the current Characterization of generation of 8-m telescopes and delivering ~4x higher resolution, will open-up for the first Rocky Earth-size time the ability to directly image and characterize Earth-size planets around several stars, from 10/21 Habitable Zone Planets M dwarfs (NIR reflected light) to Sun-like stars (thermal infrared). Starting with some basic Mon. in the Solar assumptions, I will show some early thermal imaging simulations and review the various 17:25- Neighborhood with challenges that will need to be resolved to enable this breakthrough science case. Finally, I will TMT also present a concept of using an orbital LASER satellite constellation to perform high fidelity atmospheric tomography that could potentially achieve sub-photon noise corrections of the science target star in the NIR. This system would significantly lower the required integration Christian Marois time, and potentially extend the Earth-size reflected light imaging capabilities in the NIR to (National Research more massive Sun-like stars. Council of Canada) O-16 Effect of dust size and We study scattered light properties of protoplanetary disks at near-infrared wavelengths for structure on scattered- various dust size and structure by performing radiative transfer simulations. We show that light images of different dust structures might be probed by measuring disk polarization fraction as long as the 10/22 protoplanetary disks dust radius is larger than the wavelength. When the radius is larger than observing wavelength, Tue. disk scattered light will be highly polarized for highly porous dust aggregates, whereas more 09:10- compact dust structure tends to show low polarization fraction. Next, roles of monomer radius Ryo Tazaki and fractal dimension for scattered light colors are studied. We find that, outside the Rayleigh (Tohoku University) regime, as fractal dimension or monomer radius increases, colors of the effective albedo at near- infrared wavelengths vary from blue to red. Our results imply that disks showing grey or slightly blue colors and high polarization fraction in near-infrared wavelengths might be explained by the presence of large porous aggregates containing sub-micron sized monomers. O-17 Radiative scale-height The current paradigm state that planets form in young circumstellar disks called protoplanetary and shadows in disks. However, it is still difficult to catch planet formation at the act. Nevertheless, in recent protoplanetary disks years substantial evidence of the indirect presence of planet formation have been identified (by 10/22 eg., ALMA, SPHERE), such as gravitational perturbations, rings, cavities, and emission dips or Tue. shadows cast on disks. To better understand the meaning of such observations, a better 09:25- Matias Montesinos description of the vertical disk structure is needed. Typically, to model the scale-height, (Universidad de theoreticians only assume the work done by the gas pressure to equilibrate gravity, ignoring Valparaiso) radiative and turbulent pressure or magnetic fields. In this presentation, I will discuss the relevant role of radiative pressure that could arise in hot regions of ~ 1000 K or more (e.g., where proto-planet are assembled, or inner rims of young disks), describing some consequences; the puffed-up material in the vertical direction of hot protoplanets -able to cast shadows-, and the 'extremely' high aspect-ratio (~ 0.2) observed at the inner rim of some circumstellar disks. O-18I Observing planet Planets form in gaseous protoplanetary disks surrounding newborn stars. As such, the most formation in direct way to learn how they form from observations, is to directly watch them forming in disks. protoplanetary disks In the past, this was difficult due to a lack of observational capabilities, and planet formation 10/22 was a subject of theoretical research. Now, thanks to a fleet of new instruments with Tue. unprecedented resolving power that have come online in the past decade, we have started to 09:40- Ruobing Dong unveil features in resolved images of protoplanetary disks, such as gaps and spiral arms, that are (University of Victoria) most likely associated with embedded (unseen) planets. By comparing observations with theoretical models of planet-disk interactions, the properties of these still forming planets may be constrained. Such planets help us test planet formation models. I will introduce the current status of this field, and highlight some of the latest developments. O-19I Small-scale The process of disk evolution and planet formation will leave an imprint on the distribution of Substructures in solid particles at different locations in a protoplanetary disk, resulting in a variety of Planet-forming Disks substructure over large and small scales. The focus of recent ALMA observations at high 10/22 resolution has been to characterize the underlying substructure of these disks, from dust Tue. continuum and gas tracer images with a few AU spatial resolution. In this review I will discuss 11:00- Laura Perez recent results, focusing on the DSHARP survey results and including those circumstellar disks (Universidad de Chile) around young stars in multiple systems. O-20 Dust Filtration in T HP Cha is known to be a triplet system belonging to Chameleon I star-formation region (age: Tauri Star HP Cha ~2Myr), and the primary star is classified as T Tauri star with a distance of 190 pc (Gaia DR2). The dust emission has been detected in ALMA Band 3 (Dunham et al. 2016) and Band 7 (Long 10/22 et al. 2017), but failed to resolve disk substructures such as a cavity and gaps due to the large Tue. Mihoko Konishi beam size although the observed visibilities show a high possibility of harboring substructures. 11:40- (Oita University) To discover disk substructures and to compare the dust spatial distribution at multi- wavelengths, we observed HP Cha system with ALMA and VLT/SPHERE. Our ALMA

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observations (project code: 2017.1.01460.S) were conducted at Band 6 to detect dust continuum and CO gas isotopes. In addition, we obtained the scattered light from the disk with IRDIS DPI (differential polarimetric imaging) mode in J band, and searched point-like sources by using IFS in broad band (YJH) and IRDIS DBI (dual band imaging) mode in K1K2 band (program ID: 0102.C-0561). The 1.3 mm continuum image (beam size: 53 mas x 30 mas) first revealed a ring structure with the width of ~0.1 arcsec (~19 au) at the radius of ~0.27 arcsec (~51 au), while the polarized light was detected within ~0.23 arcsec (~44 au). The results indicate the clear evidence of dust filtration in HP Cha disk. We will discuss the detail properties and origins of observed dust distribution. It is noted that there is no point-like source detected in both ALMA and SPHERE images. O-21 The illusive disk Debris disks can be seen as the left-overs of giant planet formation and the possible nurseries of around TWA 7 rocky planets. While M-type stars out-number more massive stars we know very little about the time evolution of their circumstellar disks at ages older than 10 Myr. While sub-millimeter 10/22 observations are best to provide first order estimates of the available mass reservoir (and thus Tue. Amelia Bayo better constrain the evolution of such disks), high-angular resolution∼ near-infrared polarimetric 11:55- (IFA / NPF) observations provide extremely complementary information about the dust properties. Here, we present ALMA Cycle 3 Band 7 observations of the debris disk around the M2 star TWA7, which had been postulated to harbor two spatially separated dust belts, based on unresolved far- infrared and sub-millimeter data. We show that most of the emission at wavelengths longer than 300 µm is in fact arising from a contaminant source, most likely a sub-mm galaxy, located at about 6.6″ East of TWA 7 (in 2016). Fortunately, the high resolution of our ALMA data allows ∼us to disentangle the contaminant emission from that of the disc and report a significant detection of the disk in the sub-millimeter for the first time with a flux density of 2.1±0.4 mJy at 870 µm. With this detection, we show that the SED can be reproduced with a single dust belt. Finally we will discuss the complementarity of VLT/SPHERE polarimetric observations of this disk. O-22I Optical and near- The past five years have seen a revolution in our understanding of the earliest phases of planet infrared scattered light formation. While in previous decades disks were assumed to be smooth, we now see that imaging of distinct features such as rings and spirals are ubiquitous. The extreme adaptive optics imager 10/22 protoplanetary disks SPHERE at the ESO/VLT is one of the flagship instruments for obtaining scattered light Tue. observations of circumstellar disks. I will give an overview of the the current status of the field, 13:30- with particular focus on the results of the SPHERE consortium guaranteed time survey. I will Christian Ginski review what we have learned about planet formation in the first 10 Myr of disk lifetime so far (Anton Pannekoek and how our results compare to ALMA (sub)mm observations of dust continuum emission. Institute for Astronomy, Moving forward from the initial surveys, some of the key questions that we want to answer in Amsterdam) the next years are: How is the appearance of disks in scattered light linked to disk evolution and stellar mass? Are the disk features that we detected around many intermediate mass stars equally present in lower mass systems? Are certain features common at similar system ages? And how may all of this link with planet formation? I will discuss how we plan to address these questions and our current instrumental limitations. I will also demonstrate the importance of new observation modes and data reduction techniques to hunt for embedded protoplanets. O-23I Near-infrared high Protoplanetary disks show complicated structures such as multiple rings and spiral arms. On the resolution observations other hand, some disks have a relatively simple structure, i.e., a single ring and /or a crescent of protoplanetary disks structure. Such a simple disk can be easily characterized by a simple modeled disk, which could 10/22 with Subaru allow us to investigate correlations between disk properties such as a depth of cavity and a disk Tue. size. During the SEEDS (Strategic Explorations of Exoplanets and Disks with Subaru) project 14:10- in 2009-2015, we have conducted near-infrared high resolution observations of disks mainly Jun Hashimoto with such a simple structure. Thanks to a better performance of the polarimetric difference (NINS) imaging technique, we detected about 50 disks among 79 YSOs. In my talk, I will review major discoveries in the SEEDS disk survey. Furthermore, I will talk about comparisons between SEEDS and ALMA disks. To date ALMA has observed more than 50 disks with a simple structure. We have performed modeling efforts in 51 simple ALMA disks. I will discuss about correlations of physical properties in SEEDS and ALMA disks. Finally, I will mention future plans of a possible disk and planet survey with Subaru. We will install the near-infrared wavefront sensor and new polarimetric mode into extreme AO system SCExAO, which allows us to probe disks and planets around faint objects such as M type stars. O-24I A polarized view of Polarization is an essential aspect of high-contrast imaging, both in terms of scientific yield as high-contrast imaging well as optical performance. First of all, most of our targets are polarized in visible and near-IR light, as they reflect/scatter starlight. This enables us to distinguish faint exoplanets and 10/22 circumstellar disks from the bright residual halo of starlight that is generally unpolarized.

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Tue. Frans Snik Moreover, the polarization of these objects as a function of wavelength and phase angle 16:00- (Leiden Observatory) provides crucial and unambiguous information about, e.g., atmospheric constituents and dust properties. Even biomarkers are accessible through polarimetry, e.g. linearly polarized O2 spectral features and circular polarization signals due to homochiral molecules. Secondly, in addition to introducing instrumental polarization effects that degrade the polarimetric performance, polarization effects of optical components may either deteriorate or boost the contrast. Every reflection and refraction can induce polarization-dependent phase and amplitude structure in the pupil. These polarization aberrations need to be understood and mitigated at the fundamental level to ensure full control of the PSF for coronagraphy and polarimetry. On the other hand, novel liquid-crystal technology and polarization tricks allow for the design and construction of broadband coronagraphs (like the Vector Vortex Coronagraph and the vector Apodizing Phase Plate) that can combine high-contrast performance with (spectro-)polarimetry. I will provide an overview of polarimetric techniques and technology that are currently implemented in the ground-based high-contrast imagers SPHERE, GPI and SCExAO, or are considered for their upgrades. I will introduce system-level solutions for polarimetry with future space telescopes. Finally, I will present two polarimetric instruments that we are building for observations of the Earth-as-an-exoplanet from orbiting platforms (which includes the ISS and the moon) to provide benchmark data for future direct characterization of Earth-like exoplanets. O-25 Polarization-dependent To directly image Earth-like planets in (polarized) reflected visible light, future space-based beam shifts upon telescopes and 30-m class ground-based telescopes and instruments need to reach extreme metallic reflection in contrasts. The polarimetric and coronagraphic performance of these telescopes and instruments 10/22 diffraction-limited will be limited by polarization aberrations, i.e. minute polarization-dependent wavefront errors Tue. astronomical telescopes resulting in polarization structure in the point spread function (PSF). These polarization 16:40- and instruments aberrations can be modeled with polarization ray tracing codes (e.g. Breckinridge+2015), but such numerical codes give little insight into the full range of effects and their origin. Here we show that the predominant polarization aberrations induced by metallic reflection can be Rob van Holstein described as four polarization-dependent shifts of the light beam. These spatial and angular (Leiden Observatory) Goos-Hänchen and Imbert-Federov shifts have been extensively studied by the physics community and can be described with closed-form mathematical expressions. We explain the origin of each shift and quantify their size as a function of angle of incidence for different materials. Two of the four effects laterally shift the PSF in the focus, thereby misaligning the orthogonally polarized beams. For VLT/SPHERE-ZIMPOL this significantly reduces the polarimetric speckle suppression close to the star. The two high-impact beam shifts are caused by the non-zero retardance and angular retardance gradients of the mirror, while the mirror’s reflectance only induces a small correction to the size of these shifts. Because the beam shifts cannot be easily mitigated through calibration and data reduction, future designs of optical systems should more strongly focus on limiting the retardance (gradients) rather than just optimizing the reflectance for high throughput. We apply this lesson to SPHERE-ZIMPOL in light of the proposed SPHERE+ upgrade. The insights from our study can be applied to improve the performance of many future and proposed space- and ground-based high-contrast imagers and polarimeters, such as WFIRST, LUVOIR, HabEx, ELT/PCS (EPICS) and TMT/PSI. O-26I Revealing exoplanet High-resolution spectroscopy is a robust and powerful tool for characterising exoplanet atmospheres by atmospheres. Key to its success is its ability to resolve molecular spectral features into a dense combining high forest of thousands of individual lines that are arranged in unique patterns. The technique was 10/22 contrast imaging with initially used to detect molecules in a hot Jupiter atmospheres, relying on the large Doppler shift Tue. high resolution of a planet during its orbit to disentangle its spectrum from the glare of its host star. However, 17:10- spectroscopy more recently, it has been used in combination with high contrast imaging to reveal the atmospheres of long orbit, young giant exoplanets. The technique is sensitive to the depth, shape, and position of a planet’s spectral lines. This means not only has it revealed the planet’s Jayne Birkby composition, but also its radial velocity, and it has enabled the first measurements of a new (University of fundamental parameter of an exoplanet - its rotation period. In this talk, I will review the Amsterdam) technique of combining high resolution spectroscopy and high contrast imaging, and discuss the ground-breaking advances it has already made in the study of giant exoplanet atmospheres. I will end with details on how the technique can progress in the era of the ELTs, as well as its complementarity to JWST and other lower resolution data. I will highlight its potential for mapping giant exoplanet atmospheres and how it is being trained to be able to detect biosignatures in nearby rocky worlds in the future. O-27 The SPHERE view of We present recent SPHERE observations of the system Proxima Centauri, the closest star to our our closest multi- Sun. In 2018 we presented for the first time the determination of its gravitational mass thanks a microlensing event that happened when Proxima passed close to a background star. For this aim

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10/22 planetary system: we obtained a sequence of deep coronagraphic observations with SPHERE. We continued our Tue. Proxima Centauri intensive monitoring in 2018 and 2019, resulting in the observations of a second microlensing 17:50- event that can permit us to refine the mass estimation. We also present the search for a direct Alice Zurlo evidence of the planet (candidate?) Proxima Cen c, presented in Damasso et al., submitted, from (Universidad Diego an optimized combination of our SPHERE images to obtain the deepest detection limits Portales) O-28 Masses, Orbits, and High-contrast imaging surveys have been plagued by two major shortcomings: an inability to New Planets and Brown select pre-select targets hosting detectable planets and brown dwarfs, and an inability to Dwarfs from measure the masses of detected planets. I will show how absolute astrometry from Hipparcos 10/22 Combining Imaging and Gaia is now overcoming both problems. With astrometry, imaging, and (in some cases) Tue. with Astrometry and radial velocities, we are measuring precise masses and orbits of planets and brown dwarfs, 18:05- Radial Velocity including a 4% mass of Gl 758B and a 7% mass of Gl 229B. Despite the fact that epoch astrometry for Gaia will be unavailable for years, I will show how we can use the currently available epochs and scan angles to fit orbits nearly as well as if we had the full epoch Timothy David Brandt astrometry. We have already implemented this in a full likelihood calculation, and I will show a (University of California, suite of results. This approach, using the observation epochs and scan angles, will be critical Santa Barbara) when Gaia DR3 releases acceleration measurements in 2021. Today, there are nearly 30,000 stars showing astrometric acceleration; I will present initial results for our large-scale radial velocity follow-up program to identify the best targets for high-contrast imaging. Finally, I will present a brown dwarf discovered using radial velocities, but with an incorrect published radial velocity orbit. With the aid of Hipparcos and Gaia astrometry, we measure the brown dwarf's mass and its likely current position. This old brown dwarf is likely accessible by high-contrast imaging today and will help anchor substellar cooling models. O-29I Characterizing Directly With the conclusion of the current generation of surveys for directly imaged planets, we now Imaged Exoplanets have a firm understanding of the relative rarity of widely separated Jovian planets. At the same time, we are moving from the realm of discovery into characterization, both in terms of system 10/23 architectures and atmospheric properties for these unusual objects. Precision astrometric follow Wed. Quinn M. Konopacky up of companions for as long as a decade has led to constraints on their orbital properties, 09:10- (University of California, including possible eccentricity measurements. Spectroscopic follow-up has enabled San Diego) characterization of their atmospheric parameters, including properties that may shed light on formation pathways. In the next several years, a significant effort will focus on pushing toward observations at very high spectral resolution, where both atmospheric and kinematic information can be derived, providing a deep understanding of this fascinating planetary population. O-30 Detailed Monitoring of Since their discovery, the four planets orbiting HR 8799 have been extensively studied. Despite the HR 8799 Planets this, it has been difficult to discern differences in the atmospheric and chemical properties of the inner three planets, c, d, and e. Additionally, these planets are closely packed together, and the 10/23 latest stable orbits require the planets to be perfectly coplanar, which cannot be completely true. Wed. Jason J. Wang To address the first question, we used the CHARIS integral field spectrograph behind the 09:50- (Caltech) SCExAO adaptive optics system to obtain 17 hours of simultaneous J- through K-band low resolution spectra of HR 8799 c, d, and e over the course of two nights. We see clear spectral differences between the three planets, indicative of differences in atmospheric chemistry. We developed a technique to search for atmospheric variability to overcome calibration issues with coronagraphs and I will present the latest results. To constrain the orbital configuration, we made the first long-baseline interferometric detection of an exoplanet when we detected HR 8799 e with VLTI/GRAVITY. Using baselines up to 130 m, we are measuring the positions of the planets to 100 microarcsecond precision, a factor of 10 better than previous measurements. A single epoch has ruled out perfectly coplanar stable orbital solutions, and I will discuss the prospects of additional dynamical constraints with an upcoming orbital monitoring campaign. O-31 Moderate Resolution Recent direct imaging of exoplanets has revealed a population of Jupiter-like objects that orbit Spectroscopy of at large separations (~10-100 AU) from their host stars. These planets, with masses of ~2-14 Directly Imaged MJup and temperatures of ~500-2000 K, remain a problem for the two main planet formation 10/23 Exoplanets models—core accretion and gravitational instability. We present results from our ongoing Wed. survey of directly imaged planets with moderate (R~4000) spectral resolution. We are making 10:40- use of OSIRIS on the W.M. Keck I 10 meter telescope, which offers some of the best spectra to- Kielan Kathryn Wilcomb date for directly imaged substellar companions. Thus far, we have observed eight companions (UC San Diego) in the K band (~2.2 µm), including the “super-Jupiter” Kappa Andromeda b. Our spectra reveal resolved molecular lines from water and CO, allowing for the derivation of atmospheric properties such as temperature, surface gravity, metallicity, and C/O ratio. In particular, we confirm that Kappa And b has a low surface gravity, consistent with a young age and mass near

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the deuterium burning limit. We also find that Kappa And b potentially has a sub-solar metallicity. We compare our spectra of the companions in K band to those of other brown dwarfs and gas giant planets, and to each other. Our survey will improve our knowledge of the intricate atmospheres of young, substellar objects. O-32 Directly-imaged Inverse methods have become a fundamental analysis technique for modelling exoplanetary atmospheric atmospheres. This technique explores a variety of potential bulk and atmospheric model characterisation with parameters that combine to best-fit an observed spectrum. TauREx (Tau Retrieval of 10/23 TauREx retrievals Exoplanets) is a Bayesian retrieval suite designed to be applied to spectroscopic observations of Wed. extrasolar planetary atmospheres. We have adapted TauREx for analysis of near-infrared 10:55- spectrophotometry from a variety of directly-imaged gas giant exoplanets and brown dwarfs. Niall Whiteford This includes the HR 8799 system, Beta Pic b, 51 Eri b, and PSO 318 observed using (University of instruments such as SPHERE, GPI and GNIRS. We also perform retrieval analysis on L and T Edinburgh) dwarf spectra from the IRTF SpeX Spectral Library. This analysis returns estimates for target mass, radius, surface gravity, temperature-pressure structure and cloud properties, as well as confirming and constraining the presence of a variety of molecular species including H2O, CO and CH4. Inverse techniques have mainly been applied to transit spectroscopy in the past and as a result, this is the first application of retrieval analysis to many directly-imaged targets. This project aims to help bridge directly-imaged exoplanet observations with robust, efficient and precise characterisation. The development and adaptation of this retrieval tool is timely and relevant given the upcoming launch of JWST. In this talk I will present a summary of the novel retrieval results from this project. O-33I Using Debris Disks to More than 20% of nearby main sequence stars are surrounded by debris disks, where Trace Planetary System planetesimals, larger bodies similar to asteroids and comets in our own Solar System, are Formation and ground down through collisions. Debris disks represent the end-stage of circumstellar disk 10/24 Evolution evolution, composed of remnant material that provides a fossil record of earlier planet formation Thu. processes. Planets orbiting within these disks sculpt the dust through gravitational interactions, 09:10- producing observable structures that illuminate the dynamical evolution of the system. I will Meredith Ann highlight recent work that connects observed debris disk structure to sculpting planets and MacGregor provides clues to the composition of the colliding planetesimals. Many of these results come (Carnegie Institution for from the Atacama Large Millimeter/submillimeter Array (ALMA), which has revolutionized Science, Dept. of our understanding of how planetary systems form and evolve. Going forward, connecting Terrestrial Magnetism) millimeter observations with complementary work at optical and infrared wavelengths offers us an opportunity to take a multi-wavelength view of planet formation. O-34 Debris disks imaged We summarize major results from a four-year debris disk survey of 100+ stars in NIR, polarized with the Gemini Planet scattered light with the Gemini Planet Imager Exoplanet Survey (GPIES). The survey probes Imager Exoplanet young planetary systems (10—100 Myr) for micron-sized dust on Solar System-like scales with 10/24 Survey polarimetry and high angular resolution. Among the 26 disks detected, seven are scattered-light Thu. discoveries, over a dozen are seen in polarized intensity for the first time, and all are resolved 09:50- on spatial scales of 0.5—7.0 au. We now know the detailed morphologies of these disks, a Paul Kalas handful of which either may be disturbed by interaction with hypothetical low-mass (University of California companions or have giant planets directly imaged. We link our measurements to ALMA Berkeley) observations, showing an empirical relationship between the radial locations of small and large disk grains. Our data give estimates of the disk-scattered light's polarization fraction, which is a key factor in determining grain compositions, sizes, and structures that are only weakly constrained otherwise. Thus, the GPIES disk survey pushes the bounds of theory and modeling to explain observations and will motivate the science goals of advanced instrumentation and facilities in the coming decade. This work was supported by NSF AST-1518332, NASA NNX15AC89G and NNX15AD95G/NEXSS. O-35 Analysis of the Over the past years, we have consistently re-analyzed the HST NICMOS coronagraphic archive population of debris using large multi-reference stars archival PSF libraries (MRDI) and modern PSF subtraction disks viewed with HST algorithms (PCA), as part of the ALICE program. This innovative post-processing methods 10/24 improved by a factor of 15 to 35 the point source detections limits within 1’’ from the star over Thu. previous NICMOS detection limits. Combined with the extreme sensitivity of HST to resolved 10:05- Elodie Choquet object, this method enabled us to detect 12 debris disks for the first time in scattered light. (Laboratoire These disks all present low surface brightness profiles despite moderate fractional IR d'Astrophysique de luminosities (L_IR/L_star ~ 1e-4), and add up to a growing population of faint debris disks with Marseille) scattering properties distinct from the bright archetypal systems that have been observed and characterized since the 2000s or before. From the population of 46 debris disks resolved in scattered light and the population of about 100 debris disks resolved in thermal emission, we can start comparing the properties of debris disks as a population.

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In this presentation, I will briefly review the results of the ALICE program on debris disk detections, and discuss the hit-and-missed in the larger context of the scattered-light resolved vs thermal emission-resolved debris disk populations. O-36 A Deep Polarimetric HD 106906 is a young, binary stellar system, located at ~102.8 parsecs away in the Lower Study of the Centaurus Crux (LCC) group. This system is completely unique in that it contains an Asymmetrical Debris asymmetrical debris disk, as well as an ejected 11M(Jup) planet companion, at a separation of 10/24 Disk HD 106906 ~738 AU. Only 4 other systems are known to contain both a disk and detected planet, where Thu. HD 106906 is the only one in which the planet has apparently been ejected. Furthermore, the 10:20- debris disk is nearly edge on, and extends roughly from 50 AU to >500 AU, where previous Katie Ann Crotts polarimetric studies with HST have shown the outer regions to have high asymmetry. The (University of Victoria) presence of an ejected planet sparks questions about the origin of this asymmetry. To better understand the structure and composition of the disk, deeper data have been taken with the Gemini Planet Imager (GPI), which we have used to perform a deep polarimetric study of HD 106906’s asymmetrical debris disk. The data were taken in the H-band, and supplemented with both J and K1-band polarimetric data which have been obtained through one of GPI’s Large and Long Programs (LLP). MCFOST, a 3-D radiative transfer code, has been used to model the disk in each wavelength, where the models were then compared to our data via MCMC. Polarimetry is important in the study of debris disks, as it helps us constrain their dust grain characteristics, as well as allowing us to obtain high-contrast images. By modelling the disk across several wavelengths, we have been able to better constrain both its density structural and dust grain properties. This has revealed a significant difference in the dust grains between either side of the disk; we will discuss these differences in terms of the likely dynamical evolution induced by the planet. O-37 The scattering phase Extreme AO instruments have revealed exquisite details on debris discs, allowing to extract the function of debris disks scattering phase function of the dust particles in unpolarised or polarised light. This is a powerful diagnostic tool to understand the physical properties of those particles, especially their 10/24 structure and size. This suggests we are observing fluffy aggregates rather than compact dust Thu. Julien Milli grains. 10:35- (ESO) I will review here the few disks where this information has been extracted, what was inferred, highlighting the differences and similarities between the dust properties in those systems. I will show how experimental physics but also numerical simulations and solar system science can instruct the field of debris disk science on how to interpret the dust phase functions. O-38 Exoplanet detection: A Traditional methods for post-processing of pupil tracking observations are limited in temporal approach for performance close to the inner working angle due to the larger field-rotation required to displace increasing contrast a source on the detector and the associated temporal exclusion criteria (protection angle) for the 10/24 performance close to data. We have developed a data-driven temporal systematics model based on non-local Thu. the inner working angle reference pixels that circumvents these limitations. 11:30- This model is valid under the assumption that the underlying causes of the systematics affect multiple pixels, which is generally the case for the speckle pattern in high-contrast imaging. We Matthias Samland simultaneously fit a forward model of a planet signal “transiting” over detector pixels and (Max Planck Institute for reference light curves describing the temporal trends of the speckle pattern to find the best Astronomy) fitting model describing the signal. With our implementation of a non-local, temporal systematics model, called TRAP, we show that it is possible to gain up to a factor of six in contrast at close separations (smaller 3 lambda / D) compared to a spatial model with temporal exclusion criterion. We further demonstrate that the temporal sampling has a big impact on the achievable contrast, where shorter exposure times result in significantly better contrasts. For beta Pic data taken with VLT/SPHERE at short integration times (4 seconds), the approach improves the SNR of the planet by a factor of four compared to the spatial systematics model. Finally, we show that the temporal model can be used on unregistered data which has only been dark and flat corrected without the need for further pre-processing. O-39 Beyond Gaussianity for In the field of post-processing to unveil exoplanets and disks signals within high-contrast the speckle statistics, a images, such as ADI- or SDI-based techniques, the widely used assumption is that the starlight new consensus for post- residuals follow a Gaussian statistics. However this assumption is known to be incorrect as the 10/24 processing of high- residuals actually follow a sub-exponential distribution. This wrong hypothesis affects directly Thu. contrast images. the false alarm probability and inherently the detection limits in terms of the 5-sigma contrast 11:45- curves that is currently used in publications. In this presentation, we will demonstrate that the residuals are better represented by a Laplacian distribution. From this observation, we produce Faustine Cantalloube detection maps after a PCA processing (the STIM-map) enabling automatic detection of circumstellar signals. We also modified the inverse problem expression used in the

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(Max Planck Institute for ANDROMEDA method to match the Laplacian distribution and show that it reduces the false Astronomy (MPIA)) positive rate and increases the true positive rate in the final detection map. We will conclude by presenting other innovative algorithms currently under development that are benefiting from this observation. O-40 Reconciling kernel- Coronagraphs are powerful tools to probe the direct neighborhood of stars at very high phase and contrasts. Their vulnerability to wavefront errors however makes them less efficient for coronagraphy: new observations at angular separations smaller than two or three resolution elements. In this 10/24 steps towards regime, observables robust to instrumental phase noise, like the closure- and kernel-phase Thu. combining the extracted from non-coronagraphic images, have proven capable of effectively picking up 12:00- performance of moderate contrast features down to the formal diffraction limit. opposing techniques. Direct kernel-phase analysis of coronagraphic images is unfortunately not possible in theory. The focal plane mask used in a coronagraph indeed destroys the shift-invariance properties that give meaning to the analysis of their Fourier transform. We nevertheless investigate how Romain Laugier techniques initially developed in the context of coronagraphic observations can be applied with (Universite Cote d'Azur, kernel-phase to boost the contrast detection limits. Observatoire de la Cote Firstly, we show how kernel-phase can be used on saturated images from the Hubble Space d'Azur, CNRS, Telescope and how it allowed a new detection of a companion at 1.3 lambda / D at a contrast of Laboratoire Lagrange, 55 at 2.2µm. France) Secondly, inspired by Angular Differential Imaging, we have devised a similar method called Angular Differential Kernel to remove static biases from our measurements which are a limiting factor for reaching high contrasts. We present a recent comparative on-sky analysis of its performance using the SCExAO instrument at the Subaru Telescope Finally, we show how pupil plane apodization masks can be used to locally decrease the photon noise in the images, and how their effect translates into the kernel-phase observables, therefore improving the capability of kernel-phase to detect faint companions around nearby stars. O-41I Photonics technology High-contrast instruments, especially aiming at detection and characterization of Earth-like toward high-contrast planets, require state-of-the-art and future photonics technology. In this presentation our recent imaging instruments activities, mainly two topics, will be exhibited: (1) a common-path visible nulling coronagraph 10/24 (VNC) based on birefringent prisms and (2) focal-plane mask coronagraphs based on photonic Thu. crystals. The common-path VNC has advantages of its stable interferometric output, achromatic 13:30- Naoshi Murakami nulling capability, insensitivity to pupil geometry, adjustable inner working angle and so on. (Hokkaido Univ.) The common-path VNC is compatible with a spatial light modulator (SLM) for dark-hole control to reduce residual stellar speckles. The SLM is an attractive device thanks to its large pixel format which enables us to create huge dark holes. Although it is still immature, a huge dark hole as large as roughly 100 lambda/D in radius can be created in a laboratory testbed. Furthermore, the common-path VNC coupled with an ExAO is now under construction for the segmented-mirror 3.8m Seimei Telescope, which will be a good lesson for future ELTs toward Earth-like planets around late-type stars. As the second topic, various photonic-crystal coronagraphic masks have been developed to date. These masks are composed of space-variant wave plates with extremely small manufacturing defects to control Pancharatnam-Berry’s phase. Currently an effort has been done to achromatize the masks based on multi-layer wave plates. Super-achromatic masks have been designed and fabricated both for ground-based observations in near-IR (e.g., SCExAO on Subaru Telescope), and space observations in visible for detecting Earth-like planets around Sun-like stars. Pupil apodizers have also been designed and fabricated so that these masks can be installed into arbitrary aperture telescopes. In this presentation, our recent activities toward future high-contrast observations will be exhibited. O-42 Overview and on-sky In the last few years the vector-Apodizing Phase Plate (vAPP) coronagraph has been installed results of the vector- and commissioned in high-contrast imaging (HCI) instruments on multiple telescopes, most Apodizing Phase Plate notably MagAO/Magellan (2-5μm), SCExAO/Subaru (1-2.5μm), LMIRCam/LBT (2-5μm) and 10/24 coronagraph the stratospheric balloon mission HiCIBaS (850 nm, flight August 2018). The vAPP is a single- Thu. optic pupil-plane coronagraph manufactured from patterned diffractive phase plates that apply 14:10- achromatic phase. The vAPP changes the point-spread function (PSF) to generate dark holes, David Doelman regions where the stellar diffraction halo is significantly suppressed. The vAPP provides a (Leiden Observatory) simple upgrade for high-contrast imaging systems, yet it provides contrasts of 10-5 at small inner working angles, it is extremely versatile, operates up to 100% broadband and is stable against tip-tilt jitter and resolving the star. The direct-write technology used to manufacture these vAPP coronagraphs is capable of writing extreme geometric phase patterns and consequently provides great freedom in shaping the PSF. Therefore, the vAPP can be designed to accommodate focal-plane wavefront sensing and holographic astrometric/photometric reference spots for more accurate post-processing,

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showing its versatility. We applied these techniques in the designs for Subaru/SCExAO, HiCIBaS, MagAO-X/Magellan and ERIS/VLT. The broadband nature of the vAPP makes it ideal for spectroscopy. The vAPP is able to make use of the full bandwidth of an integral field spectrograph (IFS), and two vAPPs are already installed on HCI instruments equipped with an IFS, i.e. CHARIS/Subaru and ALES/LBT. We demonstrate that data of a vAPP combined with an IFS allows for multiple post-processing methods and explain how they can be combined to optimally extract low-resolution spectra of sub-stellar companions. We show the calibration of the vAPPs installed in these instruments and present their first on-sky results and contrast curves. Lastly, we show the current status of a reduction pipeline and observation preparation tool for using the vAPP. O-43 The Phase-Apodized- The phase-apodized-pupil Lyot coronagraph (PAPLC) is a pairing of the apodized-pupil Lyot Pupil Lyot coronagraph (APLC) and the apodizing phase plate (APP) coronagraph that yields inner Coronagraph working angles as close as 1.4 lambda/D at contrasts of 10-10 and post-coronagraphic throughput 10/24 (PAPLC): a simple, of >75% for telescope pupils with central obscurations of up to 30%. PAPLC designs can be Thu. high-performance made entirely achromatic. 14:25- Lyot-style coronagraph The PAPLC works by manipulating the phase in the pupil plane to modify point spread function with a small inner (PSF), similar to an APP coronagraph. The bright side of the PSF is removed with a knife-edge working angle focal-plane mask and a Lyot stop is used to further filter out the residual stellar light. We present PAPLC designs for the VLT/SPHERE instrument and the LUVOIR-A pupil. These designs show a reduced inner working angle (by 1.0 and 1.5 lambda/D respectively) and an Emiel Por increased post-coronagraphic throughput (by 1.7x and 2.8x respectively) compared to (Leiden Observatory) preliminary APLC solutions. We present two possible implementations of the PAPLC coronagraph in a high-contrast imaging instrument. The first uses a liquid-crystal geometric-phase pupil-plane apodizer to produce two PSFs with opposite dark zones, and a focal-plane mask that blocks the bright side of each PSF. We show initial laboratory results on a purpose-built testbed in Leiden. The second implementation uses Fresnel propagation effects from two deformable mirrors instead of the phase-only apodizer. While not inherently achromatic, this still yields similar performance over large spectral bandwidths. Furthermore, we demonstrate with numerical simulations how aberrations affect contrast and how wavefront sensing can be integrated into the PAPLC to measure and counter these aberrations. By making the focal-plane mask reflective and reimaging the bright part of the PSF onto a Zernike wavefront sensor, aberrations can be measured without using any post- coronagraphic light. O-44-1 Upgrading the Gemini The Gemini Planet Imager (GPI) is the dedicated high-contrast imaging facility, located on (Joint) planet imager: GPI 2.0 Gemini South, designed for the direct detection and characterization of young Jupiter mass exoplanets. Gemini is considering moving GPI from Gemini South to Gemini North. Analysis of GPI’s as-built performance has highlighted several key areas of improvement to its detection 10/24 Jeffrey K. Chilcote capabilities while leveraging its current capabilities as a facility class instrument. We present Thu. (University of Notre the proposed upgrades which include a pyramid wavefront sensor, broadband low spectral 15:20- Dame) resolution prisms and new apodized-pupil Lyot coronagraph designs all of which will enhance the current science capabilities while enabling new science programs. O-44-2 SPHERE+, Reaching SPHERE, the extreme adaptive optics, coronagraphic and differential spectro-imager facility at (Joint) New Depths the VLT, has greatly contributed to the exploration of new and known planetary systems in direct imaging. In 5 years of operation, SPHERE has revealed stunning details of young proto- planetary and debris disks. It has enabled to characterize the orbital, atmospheric, and 10/24 Anthony Boccaletti demographic properties of young giant planets between 10 and 100 au to complete our current Thu. (LESIA, Observatoire de view and understanding of the mechanisms of formation and evolution of giant planets. Yet, 15:20- Paris) accessing the bulk of the giant planet population close to the snow line still represents a challenge in direct imaging. To really start probing this region in young planetary systems inside 10 au, higher contrasts at shorter separations are mandatory. SPHERE+ aims at building on the lessons learned from SPHERE's current limitations to significantly boost its performance to open a new, genuine scientific window in synergy with other facilities like high-resolution spectrographs, ALMA, or the ELT from the ground, and GAIA, JWST and WFIRST from space. With a minimal impact on the instrument availability, this upgraded version will provide 1) deeper contrasts closer to the optical axis, 2) higher spectral resolution for a more detailed characterization of exoplanets atmosphere, and 3) higher sensitivity to fainter/redder stars to reach a larger sample of young objects. Not the least, the

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instrumental developments for SPHERE+ will be precursor in the ELT era for a future extreme- AO planet imager (PCS-like project). Fulfilling these objectives requires a faster atmospheric correction on-axis, a more sensitive wavefront analyser operating in the infrared, and a mid- to high-resolution spectroscopic sub- system. In this presentation, we will briefly remind the achievements of SPHERE and review the key science cases for the SPHERE+ project. We will present the potential technical implementations to reach the appropriate performances. O-45 REACH: Scientific Exoplanet characterization using High-Resolution Spectroscopy (HRS) is now one of the most Overview of Extremely promising techniques to detect atmospheric molecules along side space-borne spectroscopy of High-Contrast transiting planets. To enable this, we will connect the high-contrast instrument (SCExAO) to the 10/24 Spectroscopy at the high-resolution IR spectrograph (IRD) at the Subaru Telescope, in a project named REACH Thu. Subaru Telescope (Rigorous Exoplanetary Atmosphere Characterization with High dispersion coronography). 15:45- Post-coronagraphic HRS will improve molecular species detection by significantly reducing photon noise and speckle noise at the planet position. Hajime Kawahara The REACH project weill enable several science cases. Atmospheric characterization of self- (The University of luminous planets is one of the main goals of REACH. In addition, REACH enables the efficient Tokyo) search for the molecular lines using the cross-correlation technique. One can search for various molecules in the bands (y, J, and H), such as methane, NH3 (these two can be tracers of the non-equilibirum state of the thermochemical equilibrium), and CO2 for relatively cool planet atmosphere, TiO, VO, FeH for hotter planets, as well as for water in various cases, and other minor molecules such as acetylene, HCN. The REACH project can also be used as a spectrometer for accurate radial velocimetry of a companion of a bright star. When observing the target companion in one of two channels, we can use the laser comb simultaneously using the other channel. So, the radial velocity survey of a planet around a late-type companion star of a star binary is one of the possible science cases. We also discuss the role of the REACH project as a testbed of future high-dispersion coronagraphy applications for ultimate targets such as reflected light from Earth-like planets around a late-type star, emitted light near the diffraction limit such as nearby warm Jupiters. O-46 Exoplanet Imaging The Planetary Systems Imager (PSI) is a proposed second generation instrument for the Thirty with the Planetary Meter Telescope that focuses on high contrast exoplanet imaging. Here, we describe PSI's Systems Imager potential contributions to exoplanet science in the era of ELTs. Because PSI combines science 10/24 backends providing imaging, polarimetry, integral field spectroscopy, and high-resolution Thu. spectroscopic capabilities across a wide range of wavelengths (0.6–5 μm, as well as a thermal 16:00- Rebecca Jensen-Clem channel at 10 μm), the instrument is very well suited to address major questions in the (UC Berkeley formation and evolution of planetary systems. Addressing these questions relies on our Astronomy Department) leveraging of the diffraction-limited resolution and light-gathering power of TMT, both of which will enable us to directly study gaseous, icy, and rocky planets at a range of effective temperatures. Finally, it may allow the detection of biosignatures in the atmosphere of planets in the habitable zones of nearby M dwarfs. O-47 Planet formation and Within ten years, the era of large-scale systematics surveys in radial velocity, astrometry, Exoplanets at the Era transit, micro-lensing and direct imaging will be almost complete and will provide us with a full of the Extremely Large census of exoplanetary systems within 200pc from the Sun. With the first Lights foreseen 10/24 Telescope between 2026 and 2028, the new generation of extremely large telescopes (TMT, GMT nd Thu. ELT) and planet imagers will arrive at a propitious time to exploit this large number of 16:15- discoveries. Their main objectives will be to characterize the formation, the evolution, and the Gael Chauvin physics of giant and telluric planets with the ultimate goal to search for and discover potential (International Franco- bio-signatures. In that talk, I will briefly summarize the main characteristics of the direct Chilean Laboratory for imaging instruments of the ELT dedicated to the study of disks and exoplanets, and review the Astronomy) key science cases (from the initial conditions of planetary formation, the architecture of planetary systems and the physics and atmospheres of giant and telluric planets) that they will address given their versatility and predicted performances. O-48 Overview of the The Wide Field Infrared Survey Telescope (WFIRST) Coronagraph Instrument (CGI) is a high- WFIRST Coronagraph contrast imager and spectrograph that will enable the study of gas giant exoplanets and Instrument and circumstellar disks at visible wavelengths. Future flagship mission concepts aim to characterize 10/24 exoplanet science Earth analogues with visible light flux ratios of ~10-10, and CGI is a critical intermediate step Thu. toward that goal, with predicted capability of ~10-9. CGI will have ~3 months of observing time 16:30- during the first 18 months of the mission (its "tech demo phase") to demonstrate its technology Vanessa Bailey objectives and to determine whether its as-built performance justifies additional science (Jet Propulsion Lab) observing time during the remainder of the mission. This talk will present an overview of the

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instrument, its key enabling technologies, and its operational plans, including its potential for gas giant exoplanet science. O-49I Studying Disks at High Debris disks are wonderful remote geological laboratories that provide crucial information on Contrast with the chemistry and environment of rocky and icy bodies in a planetary system. As such, they can WFIRST/CGI give astronomers a tool for understanding the formation and evolution of planetary systems as 10/24 well as a way to map our nearest stellar neighborhoods. The Wide Field Infrared Survey Thu. Telescope (WFIRST) coronagraphic instrument (CGI) will be capable of directly imaging a 16:45- John Henry Debes wide range of circumstellar disks in a combination of total intensity and polarized visible light, (STScI) improving on previous high contrast imaging by orders of magnitude. Debris disks that are a few times brighter in surface brightness than both the zodiacal cloud and the Kuiper belt will be detectable around nearby stars with the CGI, laying a path for the exploration of inner planetary systems during the WFIRST mission. We review the feasibility and potential scientific return with the expected CGI complement of coronagraphic masks and observing modes, and identify key observations that could be proposed either during the technology demonstration phase of the mission or during its later phases. O-50 The Bright Future of The Magellan Giant Accreting Protoplanet Survey (GAPlanetS) is the most sensitive high- Protoplanet Direct contrast imaging survey for actively forming planets to date. Conducted over 5 years (2013- Imaging - Lessons 2018) and with over 75 hours of open shutter time on 15 of the brightest transitional disks, this 10/25 Learned from the First survey pioneered the H-alpha differential imaging technique. With three accreting companions Fri. Generation Magellan (two protoplanets and one low mass stellar companion) successfully detected within the 09:10- Giant Accreting relatively small sample (detection rate of 20%), the GAPlanetS results highlight the bright Protoplanet Survey future of protoplanet direct imaging. I will present aggregate statistics and results of the full (GAPlanetS) survey, including reprocessings under a unified and robust framework of the three previously- published GAPlanetS detections (LkCa 15 b, PDS 70 b, HD142527 B), as well as important limits on the presence of accreting planets in gapped disk systems such as TW Hya. I will Katherine Brutlag discuss in detail lessons learned about the stability of PSF subtraction techniques in the low Follette Strehl ratio regime, and will present several new tools for analysis and optimization of direct (Amherst College) imaging data that are particularly powerful in this regime. I will end by discussing the next generation of ground and space based protoplanet imaging technologies and instruments, including MagAOX and WFIRST. O-51 Young Suns Exoplanet Many large-scale direct imaging surveys for extra-solar planets are plagued by three problems: Survey (YSES) reveals (i) The estimated exoplanet masses are strongly limited by uncertainties in the age of the planets, brown dwarfs, system, (ii) the statistical significance is diluted by the wide range of stellar masses selected, 10/25 and disks in Sco-Cen and (iii) many wide orbit companions remain undiscovered as they are often considered Fri. unlikely to be bound and therefore not scheduled for follow-up observations. 09:25- We overcome these issues by observing a unique sample of 72 solar-mass members of the Alexander Julian Bohn approximately 16 Myr-old Lower Centaurus-Crux subgroup of the Scorpius-Centaurus (Leiden University) association (Sco-Cen). We obtained two minutes total integration for each of the 72 targets using VLT/SPHERE/IRDIS in combination with an apodized pupil Lyot coronagraph. We construct a reference library of point spread functions from all the observed target stars and apply principal component analysis to remove the effects of the stellar halo. Despite the very short integration time, we are able to detect 10 Jupiter-mass objects at separations of 0.2 arcseconds and in the background limited regime we are sensitive to companions with masses as low as 3 Jupiter masses. The first epoch observations already reveal a shadowed transition disk around Wray 15-788 that shows signs of ongoing planet formation. Second epoch observations of only five systems confirm two sub-stellar companions at wide separations (>150au) by common proper motion analysis. Comparison to evolutionary models of sub-stellar objects provides preliminary estimates of approximately 13 and 25 Jupiter masses. With additional follow-up observations of the remaining 49 systems that host low-mass companion candidates, our survey will finally provide a complete census of wide orbit sub- stellar companions to a statistically highly significant sample of young, solar-type stars. O-52 A tentative first direct Within the SHINE survey and the disk part of the Sphere consortium survey on the SPHERE detection of a high-contrast imager at VLT we followed up on a very young star with sub-stellar companion. circumplanetary disk We can clearly show the companion to be co-moving, having a mass close to the deuterium 10/25 burning limit from atmospheric model fitting and additionally exhibiting strong accretion Fri. signatures, easily visible by strong Halpha flux emission with respect to the remaining 09:40- Tobias O. B. Schmidt spectrum. (Hamburg Observatory, We recently performed polarimetric follow-up and besides the detection of a disk around the Hamburg, Germany) primary star, we could identify the degree and angle of linear polarization of the companion to

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differ strongly from the primary star’s and from the expected polarization of an unrelated object. A tentative elongation, as sign of the direct visibility of the circumsecondary material allows for a unique opportunity for further follow-up of this planet candidate with disk and would be a source of so far unexploited information on planetary / brown dwarf formation. O-53 VISIR/NEAR, a 100- In June 2019, ESO and the Breakthrough Initiatives carried out the NEAR experiment, a 100- hour direct imaging hour campaign to search for low-mass planets in the Alpha Centauri system, utilizing high- search for low-mass contrast imaging in the thermal IR. This has been made possible by moving VISIR to the VLT- 10/25 planets in alpha UT4 and using the Deformable Secondary Mirror for AO and N-band AGPM coronagraphy. Fri. Centauri We will present the NEAR concept, and report on the achieved sensitivity and contrast. The 09:55- expected performance of NEAR will allow us to probe down to the mini-Neptune range, while reaching down to a true Earth analogue would require a more sensitive detector technology and Markus Kasper multiple telescopes observing in concert. We will report on the data reduction efforts carried out (ESO) by several independent teams, and present preliminary campaign results. We will finally comment on the NEAR science demonstration programme and prospects for future use of this exciting oberving capability. O-54I The Next Generation of Over the past 5 years, systems such as SPHERE and GPI have provided the first demonstrations Exoplanet Direct of low residual wavefront error, high Strehl corrections and deep planet-to-star contrasts that Imaging with Extreme reveal hitherto unseen planets at sub-arcsecond separations. In this talk, I describe progress with 10/25 Adaptive Optics the next generation of extreme AO systems, focusing primarily on the Subaru Coronagraphic Fri. Extreme Adaptive Optics project (SCExAO). SCExAO leverages in advances in wavefront 11:00- sensing and control to yield near-IR Strehl ratios in excess of 90%, yielding new sharp images Thayne Currie of known exoplanet systems. I describe how SCExAO clarifies the properties of controversial (NASA-Ames Research systems -- kappa And and LkCa 15. SCExAO, along with other upcoming systems like Center) MagAO-X and KPIC, serve as incubators for technology that will one day allow us to image an Earth in reflected light around nearby low mass stars with Extremely Large Telescopes. O-55 Thermal-Infrared Our team recently completed building —within the LBTI infrastructure— an IFS optimized for Integral Field exoplanet direct imaging. The instrument, dubbed the New Arizona Lenslets for Exoplanet Spectroscopy of Planets Spectroscopy (NALES), builds upon the successes of an earlier prototype instrument (ALES) 10/25 and Protoplanets built in 2015. NALES is uniquely powerful for exoplanet direct imaging because it is the only Fri. IFS operating in the thermal-IR where cool exoplanets peak in brightness. By probing the peak 11:40- of exoplanet SEDs NALES provides the best constraints on exoplanet luminosities while Jordan Michael Stone simultaneously covering the fundamental transitions of both CH4 and CO. Consequently, (University of Arizona) NALES also provides the most sensitive probes of the physical processes sculpting exoplanet carbon chemistry. I will present preliminary science results with NALES including observations of both directly imaged companions and a candidate companion discovered within a protoplanetary disk. I will also discuss our progress incorporating multiple coronagraphs within NALES to further increase our high-contrast performance. O-56 Directly Imaging With the launch of the JWST, the astronomy community will gain an invaluable tool for the Exoplanets and Disks detection of exoplanets and characterization of their atmospheres. The unique combination of with JWST NIRCam JWST's unprecedented sensitivity, angular resolution, and broad wavelength coverage (1 – 28 10/25 microns) has generated much enthusiasm within the high contrast imaging community, Fri. including a dedicated Early Release program along with multiple complementary GTO 11:55- Jarron Leisenring programs. These programs encompass observations of exoplanets and disks inaccessible by (University of Arizona) current ground-based AO systems. In this talk we will discuss exoplanet/disk science objectives covered by the NIRCam GTO programs, including: 1) coronagraphic imaging of debris disks; 2) exoplanet searches down to Neptune masses; 3) survey of nearby M Dwarfs; 4) characterization of known exoplanet hosts; and 5) imaging of YSO disks and protoplanets. These programs are only possible due to the high thermomechanical stability of JWST, which will ensure extremely small variations in wavefront error (1-3 nm) over a typical observation period (~3 hours), delivering an extremely stable PSF to NIRCam. We will present results from simulations using open-source Python tools (pyNRC) developed by the NIRCam Science Instrument Team for proposal planning. In addition, we will discuss lessons learned and best practices critical for effective strategies for proposal submissions, including spectral type matching of science and reference targets and the pros/cons of NIRCam direct imaging compared to coronagraphy. NIRCam's wavelength coverage offers an exciting opportunity to disentangle the effects of temperature, clouds, and chemistry in the atmospheres of extrasolar giant planets; characterize accretion onto forming protoplanets; and probe ice lines and substructures for resolved disks.

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No facility will compete with NIRCam at separations >0.75" until the ELTs late into the next decade. O-57 The Decadal Survey The NASA Exoplanet Exploration Program’s Decadal Survey Testbed (DST), one of three Testbed: coronagraph testbeds in the High Contrast Imaging Testbed facility at the Jet Propulsion Demonstrating Laboratory, aims to demonstrate the coronagraph technologies required to directly image and 10/25 Technology for characterize Earth-like exoplanets with future NASA space telescopes. The DST demonstrated Fri. Imaging Earth-like what is arguably the best performing Lyot coronagraph in the world, using two deformable 13:30- Exoplanets with Future mirrors, a Nickel-on-glass occulting spot, and annular Lyot stop to provide a 360° dark hole Space Telescopes between 3 to 9 λ/D at 550 nm. Commissioned in early 2019, the DST has become NASA’s most sensitive coronagraph testbed with a vacuum environment, high thermal/vibrational stability, and wavefront control algorithms achieving repeatable convergence below 5e-10 mean contrast Garreth Ruane within a spectral bandwidth of Δλ/λ=0.1. This testbed is now available to all principal (Jet Propulsion investigators awarded openly-competed NASA Strategic Astrophysics Technology grants. In Laboratory) this talk, I will describe the testbed design, raw contrast results in both monochromatic and polychromatic light, empirical testbed stability, current testbed limitations, and plans for future experiments. O-58 Laboratory The detection and characterization of exo-earths calls for very large diameter telescopes and the demonstration of high use of segmented primary mirrors. The additional complexity stemming from the geometrical contrast imaging on structure of such telescopes, including segment gaps, secondary obscuration and support 10/25 segmented apertures: spiders, introduces challenges into high-contrast imaging. To demonstrate capabilities for high Fri. Results from STScI contrast on these challenging apertures, the High-contrast image for Complex Aperture 13:45- HiCAT testbed Telescopes (HiCAT) testbed explores solutions in coronagraphy and wavefront sensing and control. This ongoing technology program aims to mature designs of the Apodized Pupil Lyot Coronagraph (APLC), which is currently the leading architecture for starlight suppression on Iva Laginja large segmented telescopes such as the Large UV, Optical, IR telescope (LUVOIR) in its on- (Space Telescope axis “A” configuration design. This includes the demonstration of coronagraph mask Science components, specifically the shaped-pupil APLC masks optimized for segmented apertures and Institute/ONERA) fabricated as carbon nanotube patterns on silicon substrate. Three deformable mirrors, two continuous and one segmented, are used for the demonstration of integrated wavefront control of phase and amplitude on segmented apertures. This presentation will summarize our team’s results thus far and present the latest laboratory results from HiCAT. O-59 NASA’s S5 Starshade Starshades, or occulters external to telescopes, are a promising technology for high-contrast Technology imaging and spectroscopy of distant planetary systems. Unlike coronagraphs, which employ Development Activity amplitude or phase modulating elements within the telescope to prevent starlight from reaching 10/25 the detector, starshades cast a deep shadow on the telescope’s entrance aperture, preventing the Fri. starlight from entering the telescope at all. This dramatically relaxes the performance 14:00- Phil Willems requirements on the telescope, at the price of placing the occulter on a spacecraft separate from (NASA Jet Propulsion the telescope and flying in formation with it. NASA is currently considering space telescope Laboratory) missions that use starshades for exoplanet imaging and spectroscopy. NASA also funds the development of starshade technology to bring it to sufficient maturity for such missions. We give an overview of the working principles of starshades, and present the plan and recent results of the Starshade to Technology Readiness Level 5 (S5) activity. O-60 Laboratory The primary challenge faced by extreme coronagraphy is mitigating phase errors introduced demonstration of 1e-10 into the wavefront by aberrations in the optical system or non-uniform indices of refraction in contrast with a sub- the atmosphere. External occulters, or starshades, mitigate this issue by destructively interfering 10/25 scale starshade external starlight at a large distance from the telescope. This provides a large propagation distance for Fri. occulter phase deviations to even out and extinguishes the starlight before it ever enters the telescope, 14:15- making aberrations in the optical system irrelevant. The high throughput and broadband nature of starshades make them a leading technology to enable the spectroscopic characterization of Anthony Harness Earth-like exoplanets. (Princeton University) Due to the large sizes and separations involved in the architecture of an external occulter, it is impossible to test a flight-size system on the ground and we must rely heavily on optical models to predict on-orbit performance. The validation of these optical models is critical to the success of a future starshade mission and a testbed at Princeton University has been developed to validate the models by testing 1/1000th-scale starshades. This presentation reports on the latest results of high contrast demonstrations with sub-scale starshades; an effort conducted under the Starshade Technology Activity (S5). We demonstrate 1e-10 contrast at the inner working angle of a starshade with a flight-like Fresnel number at multiple wavelengths spanning a 10% bandpass. We show that the contrast is limited by non- scalar diffraction as light propagates through the narrow gaps between starshade petals and we

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present an optical model capable of reproducing these effects. We also present the first results of testing starshades with intentional defects built into their shape to conduct a sensitivity analysis of our optical models. O-61I Direct Imaging and Coronagraphic imaging and direct spectroscopy of young planets with the James Webb Space Spectroscopy of Telescope (JWST) will add new insights into our understanding of the formation and evolution Exoplanets with the of exoplanets. I will give a brief summary of the direct imaging modes observing of the four 10/25 James Webb Space JWST instruments and present discuss how JWST will address key questions in exoplanet Fri. Telescope research: 15:15- • What are the physical and chemical processes at work in the atmospheres of exoplanets? • How does atmospheric composition vary as a function of key exoplanet characteristics, such Charles Beichman as mass, radius, level of insolation and location within the planetary system? (NASA Exoplanet • What can we learn about the formation of exoplanets from, for example, differences in their Science Institute) atmospheric carbon-to-oxygen (C/O) ratios or overall metallicities compared to those of their host stars? • Do massive planets found on distant orbits (>10 AU) have a different formation mechanism, e.g disk fragmentation vs. core accretion, compared to those on closer orbits? • Can we distinguish between ``hot start'' vs. ``cold start'' (low vs. high initial entropy) states for forming massive planets to test different formation mechanisms? • How does the presence of planets affect the structure of circumstellar disks? Can we locate unseen giant planets by studying their gravitational affects on disk systems imaged with HST, ALMA, and by JWST itself? • What can the composition of circumstellar disk material tell us about the formation of planets? • Do young planetary systems with known massive planets also contain lower mass planets? O-62I High Contrast Imaging To prepare for the upcoming launch of JWST, a broad range of proposals have been selected by of Exoplanets and STScI under the Director’s Discretionary Early Release Science (ERS) Program. Our accepted Exoplanetary Systems 52-hour JWST ERS program will directly characterize two recently-discovered, directly imaged 10/25 with JWST planetary mass companions over their full spectral range from 2- 28 microns using photometry Fri. and spectroscopy. Ours will be among the first-ever observations of bona fide exoplanets at 15:55- these wavelengths, and will be crucial test cases for atmospheric retrieval codes that have Sasha Hinkley mostly operated in the visible and near-infrared. Further, our program will demonstrate the (University of Exeter) degree to which atmospheric abundance analysis can be obtained from JWST spectroscopy, possibly providing clues to the planet formation process. As a bonus, our program will also perform deep, near-infrared, Sparse Aperture Masking on an exoplanet host star, as well as imaging of a debris disc in the thermal infrared sampling the 3 micron water ice feature. Within the first few months of JWST operation, our program will rapidly produce publicly- available datasets in modes to be commonly used by the exoplanet direct imaging communities. In addition, I will describe how our team of 120 investigators will deliver science enabling products to empower a broad user base to develop successful future JWST investigations dedicated to direct-imaging surveys for low-mass exoplanets (e.g. Saturn mass) in Cycle 2 and beyond. O-63-1 Searching and One of the key scientific objectives future NASA astrophysics flagship missions is the detection (Joint) characterizing and characterization of the earth-like planets around nearby stars using the direct imaging exoplanetary gems with technique. As a results, dedicated exoplanet instruments are being studied for the Large ECLIPS, the LUVOIR UV/Optical/Infrared Surveyor (LUVOIR) and the Habitable Exoplanet Imager (HabEx) mission 10/25 coronagraph concepts. In this talk I will discuss the Extreme Coronagraph for Living Planetary Systems Fri. instrument. (ECLIPS) instrument the LUVOIR. ECLIPS will be capable of providing starlight suppression 16:35- levels of ten orders of magnitude in multiple band-passes over a broad range of wavelengths in order to detect and characterize the light reflected from potential earth-twins. It will also allow Laurent A. Pueyo future astronomers to study in great detail the diversity of exoplanets. (STScI) First, we review the main science drivers and emphasize those that are the most stressing on the instrument design. We then present the overall parameters of the instrument (general architecture and back-end camera). We delve into the details of the static coronagraph masks, which will have the most significant impact on the total scientific productivity of the mission, and discuss in detail the choices the LUVOIR team made in order to maximize the exo-earth candidates discovery yield. We then present our work on the technological feasibility of such an instrument, focusing in particular on the ultra-stability necessary in order to achieve ten orders of magnitudes of starlight extinction over the hours of exposure that are needed to observe faint exoplanets. We present our error budget and show that using a combination of instrument level (Low and High Order wavefront sensors) and observatory level (edge sensors, laser assisted measurements) telemetry can yield an overall architecture that meets these requirements.

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Finally, we discuss of potential future technology development efforts that will mature these technologies. O-63-2 High Contrast The Habitable Exoplanet Observatory (HabEx) is a candidate large space-based strategic (Joint) Observations with the mission studied by NASA and the astrophysics community in preparation for the 2020 Habitable Exoplanet Astrophysics Decadal Survey. The baseline architecture for HabEx is a 4-meter diameter Observatory (HabEx): telescope that is designed to be the Great Observatory of the 2030s, a successor to the Hubble 10/25 Science Goals and Space Telescope (HST) with considerably enhanced imaging and spectroscopic capabilities in Fri. Projected Capabilities the ultraviolet, optical, and near-infrared. Such an observatory enables a broad range of physics 16:35- of the cosmos, cosmic origins, exoplanet exploration, and solar system science. An essential goal and driving requirement for HabEx is, for the first time, to map and spectrally characterize Bertrand Mennesson entire nearby mature planetary systems, including detailed spectra of potentially habitable (Jet Propulsion planets in these systems. The HabEx baseline architecture is optimized to reach that goal and Laboratory) includes two complementary starlight suppression systems: an internal coronagraph, primarily used for exoplanet detection and orbit determination through multiple visits, and an external starshade, primarily used for detailed spectral characterization from 200 nm to 1800 nm. Over 2.5 years of direct exoplanet observations around nearby FGK stars, HabEx is expected to measure the orbits and detailed reflected light spectra of nearly 200 planets spanning a wide range of physical separations and sizes, including dozens of rocky worlds. HabEx coronagraph system is baselining (i) a vector vortex mask with a small inner working angle and high resiliency to low-order aberrations, and (ii) a highly sensitive Zernike wavefront sensor and dual deformable mirror active wavefront correction system, similar to those successfully demonstrated in the lab for NASA’s WFIRST coronagraph instrument. Detailed end-to-end simulations predict that the HabEx telescope and coronagraph system will reach raw contrasts of a few 10-10 at separations of 3l/D, as demonstrated in the lab with a simple Lyot coronagraph and a clear (HabEx-like) aperture. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.

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Poster Abstracts

Exoplanet Imaging No. Title Abstract Time Name (Affiliation) P1-01 Characterizing a Kappa And b was discovered in the SEEDS survey and follow-up observations have been directly-imaged planet conducted for its characterizations. We present the latest Kappa And b observations with Kappa And b with Subaru/SCExAO+HiCIAO HY-bands imaging and Subaru/SCExAOI+CHARIS JHK-bands SCExAO low-resolution spectroscopy. By combining our results with previous studies we investigated Kappa And b's spectrum and Taichi Uyama performed orbital fitting, which suggests that Kappa And b is likely an L0-L1 object and has an (Caltech/IPAC, NASA eccentric orbit. Our results promote following observations with TMT for further discussions of Exoplanet Science formation/evolution scenarios of Kappa And b. Institute) P1-02 Gemini Planet Imager From the Gemini Planet Imager Exoplanet Survey, we present new near-infrared spectroscopy Spectroscopy of the of HD206893 B, a substellar companion orbiting within the debris disk of an F5V star. New J, Reddest Known H, K1, and K2 spectra with GPI demonstrate the extraordinary red color of the object, Substellar Companion presenting a challenging atmosphere to model with existing model grids. We present HD206893 B comparison with peculiar field and young L-dwarfs to assess whether the NIR spectra are consistent with upper atmosphere sub-micron hazes. Multi-epoch astrometric monitoring of the system suggests a probable semimajor axis of 10 au, well within the currently estimated disk Kimberly Ward Duong inner radius of ~50 au. As one of few systems with substellar companions imaged within the (Amherst College/Five innermost regions of a circumstellar disk, the properties of this system offer important College Astronomy dynamical constraints for companion-disk interaction and a useful benchmark for brown dwarf Department) and giant planet atmospheric study. P1-03 Spectral Multiplicity studies of stars and brown dwarfs have shown a decrease in multiplicity frequency characterization of as a function of primary mass and spectral type, with fewer multiple systems for primaries of newly detected young lower mass and later spectral types, stretching down all the way to the substellar mass-regime. substellar binaries with However, at the very bottom of the stellar and substellar initial mass function, multiplicity is not SINFONI very well-constrained. Recent efforts in associating low-mass members to young moving groups have provided much sought means to constrain ages for substellar objects, which otherwise prove difficult to do. As such, we are now at a point where we can compare the multiplicity Per Calissendorff rates for both older and younger samples of substellar brown dwarfs, which provide insight to (Stockholm University) their formation channels and dynamical evolution. This is of particular interest as very low- mass brown dwarfs are analogous to directly imaged exoplanets, which when resolved can be studied in high detail. We present the results from observations of 14 young low-mass substellar objects using the VLT/SINFONI integral field spectrograph with laser guide star adaptive optics, which we employ to detect and characterize 3 new binary systems. These results indicate for higher multiplicity frequencies for the younger populations of brown dwarfs, and that older systems may have undergone dynamical interactions disrupting the primordial binaries. By utilizing substellar theoretical models and the resolved brightnesses we obtain from our astrometric techniques, we discover some of these companions to be of planetary-mass. Furthermore, we find that the binary systems have small separations, which translates to orbital periods of just a few decades. As such, dynamical masses can be obtained within just a few years of astrometric monitoring, making these systems excellent benchmarks for calibrating evolutionary models in an otherwise scarcely probed mass-regime. P1-04 First constraints on the The SpHere INfrared Exoplanet (SHINE) GTO survey was designed to fully exploit the population of young capabilities of the new generation exoplanet imager SPHERE at the Very Large Telescope. giant exoplanets from Over 5 years, the goal of SHINE is to observe more than 500 hundred young, nearby stars to the SPHERE infrared look for sub-stellar companions and constrain the properties of their population. Deriving the survey for exoplanets frequency of the most massive planets and the lowest mass brown dwarf companions at wide (SHINE) orbital separations vs. host star mass, enables us to discern the mean outcomes of planet formation, thus defining what is extreme in the context of planetary architectures. In addition, our data provides a strong test of predictive theories of star and planet formation. In this Arthur Vigan presentation we will provide an overview of the first statistical results from SHINE, based on (Laboratoire the observations obtained on more than 150 stars. The initial results show that 1) the frequency d'Astrophysique de of gas giants around FGK (and other) stars peaks between 1-10 AU, 2) the gas giant planet mass Marseille / CNRS) function appears to be a power-law relative to host star mass, explaining the trend of gas giant detection rate with star mass and 3) the brown dwarf companion mass function is consistent

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with extrapolation from a universal stellar companion mass ratio distribution down to the minimum mass for fragmentation. We will also present a comparison of our early results with predictions of population synthesis models based on core accretion and gravitational instability in an attempt to infer the most likely formation scenario of the population of known companions. P1-05 The VIBES Exoplanet We present the ongoing VIsual Binary Exoplanet Survey (VIBES), a high-contrast imaging Survey with SPHERE survey aiming at the discovery and characterization of sub-stellar and planetary companions in young visual binary stars. Recent studies show that planet formation around multiple stars could be enhanced compared to single stars. Making use of SPHERE’s imaging and characterization Natalia Engler potential and its ability to simultaneously target all components of a stellar multiple with a high (ETH Zurich Institut for sensitivity, the VIBES survey is designed to probe the population of wide (50 – 500 AU) low- Particle Physics and mass companions to binary stars and to compare it with the occurance rate of hot Jupiters, Astrophysics) which are observed to be more frequent in multiple systems. The sample includes 27 multiples within 150 pc with ages younger than 50 Myr and a wide range of spectral types of primary stars from M0 to B8. We will discuss the preliminary results of the campaign and highlight our findings. P1-06 BEAST: The B-star The study of planetary systems in systematically different stellar environments provides an Exoplanet Abundance enhanced view of possible planetary system architectures, and can help furthering our Study understanding of planet formation and early evolution. For example, the study of planet distributions around stars of different metallicities has provided crucial clues that models based on core accretion-like scenarios are probably representative for the majority of the giant Markus Janson exoplanet demography. An equally important factor is that of stellar mass. Here, I will discuss (Stockholm University) the ongoing B-star Exoplanet Abundance Study (BEAST), which is an ESO Large Program using VLT/SPHERE for examining planetary systems around 83 of the most massive stars in the nearby and young Scorpius-Centaurus region. The first results from the survey will be presented, including the discovery of a circumbinary companion with a mass ratio to the primary system of 0.3-1%. P1-08 High Resolution Since the observation of a complex series of eclipses in the light curve of 1SWASP J140747.93- Polarisation Imaging of 394542.6 (J1407) the system has been the subject of several studies. The series of eclipses has 1SWASP J140747.93- been modelled as an enormous extra solar ring system ( 0.6 AU) around a companion, dubbed 394542.6 J1407 b, with a mass of less than 23.8 MJ . In this study we attempt to image J1407b using The Search for an polarised light in the R band assuming that the ring system∼ will produce a significant Extrasolar Ring System polarisation signal through scattering of stellar light. The observations were performed with SPHERE/ZIMPOL since it is the only extreme adaptive optics instrument in the visible that provides the resolution to detect the ring system at its expected separation of up to 5.5 AU (41 Dirk Maarten van Dam mas at 133 pc). J1407 b was not detected so a detection limit study was performed by injecting (Leiden Observatory) polarised point sources around J1407 into the data. From this study the lowest detectable polarisation degree, p, at an angular separation, αs, of 80 mas was 2.3% for a point source with a brightness contrast, ∆m, of 3 mag compared to the primary star. This raises to 6.1% for a ∆m = 4 mag source and to 15.3% for ∆m = 5 mag source. This study was compared to a radiative transfer model of the ring system, which produced a maximum p of 2.8% for a 5 mag point source at an αs of 40 mas. The model shows p decreasing with increasing separation, proving consistent with a non detection. In intensity images the limits of detection were a relative brightness of 3.5mag, which corresponds to 170.8 MJ , significantly larger than the proposed 23.8 MJ . P1-09 Imaging gap-carving, Complex spatial∼ structures in protoplanetary disks (rings, spirals, gaps) have been imaged with accreting protoplanets exquisite spatial resolution in the sub-mm and at near-IR wavelengths. They are interpreted as with MUSE signposts of planet formation. Hot, self-luminous accreting planets in young systems (typically age < 10 Myr) can be observed at moderate contrasts (~1e3 to ~1e4) in the NIR according to models of planet formation. But planets are rarely directly imaged thus far. Narrow-band Hα Julien H. Girard spectral differential imaging (SDI) is a very promising approach to detect proto-planets as it (Space Telescope allows to determine whether an object accretes and at which rate. I will present recent results Science Institute obtained with the VLT/MUSE Integral Field Spectrograph on PDS 70, the unambiguous (STScI)) detection of not one but two Hα-emitting point sources in the disk gap! The combo of a near- diffraction limited PSF and a medium resolution IFS is very powerful and a game change to detect circumplanetary accretion. P1-10 Near-visual integral- With the recent addition of the Narrow Field Mode (NFM), the Multi Unit Spectroscopic field spectroscopy of Explorer (MUSE) integral-field spectrograph now offers an AO-corrected field of view of 7.5'' the circumbinary x 7.5'' with a mean resolution of 3000 at 480-930 nm. Using MUSE in NFM we have observed planet / brown dwarf 2MASS J01033563-5515561 (AB)b, a 12-14 Jupiter mass object first discovered by Delorme et

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2M0103(AB)b with the al. (2013) orbiting two young M stars at 84 AU, and obtained a near-visual spectrum of this hot, new Narrow Field young planet / brown dwarf, in addition to resolving both components of the 0.25'' binary. Here Mode on MUSE. we present the results of our analysis of 2M0103(AB)b with one of the highlights being a very strong H-alpha emission at ~3 times continuum emission peak, possibly indicating ongoing Simon Christoffer accretion which would be unexpected for a ~10-30 Myr old object. If instead explained by Eriksson magnetic activity in the chromosphere, this level of emission would be unusually strong. (Stockholm University) P1-11 Planets and AO-fed integral field spectrographs (IFS) operating at medium resolving powers (R~5000) such protoplanets revealed as SINFONI at VLT offer to partly deblend the absorptions of cool substellar companions by the molecular (H2O, FeH, CO, CH4, NH3) at near-infrared wavelengths (1.1-2.5 µm). The molecular mapping technique. mapping technique applied to these IFS data uses correlation techniques to reveal and characterize the molecular signatures of planets in the halo of nearby bright stars. The method represent a new potential avenue to overcome the speckle noise and to perform blind searches Mickael Bonnefoy of cool companions down to a few resolution elements from nearby bright stars. (Institut de Planetologie We present a pioneering molecular mapping search for forming planets in transition disks et d'Astrophysique de previously resolved with ALMA and VLT/SPHERE (HD163296, TW Hydrae,…) using K-band Grenoble) data obtained with the SINFONI spectrograph. Contrary to traditional AO-imaging searches, our strategy allows for discriminating point-like disk structures (clumps,...) from true planetary signals. We also present new SINFONI observations of emblematic systems (HD95086, PDS70,...) aiming at re-detecting and characterizing the known companions. We will discuss the success and limitations of the technique and propose for some possible adjustments in the context of the next generation of IFS (VLT/ERIS, ELT/HARMONI, JWST). P1-12 MIRACLES: an The advent of extreme AO assisted high-contrast imaging instruments has provided detailed atmospheric insight into the atmospheric characteristics of low-mass companions at near-infrared characterization survey wavelengths (1-2.4 micron). Along the spectral sequence towards later type objects, of planetary and atmospheres emit the majority of their photons at mid-infrared wavelengths beyond 3 micron, a substellar companions regime which is expected to provide complementary information about the atmosphere's at 4-5 micron chemical abundances and cloud configuration. To better understand the characteristics of directly imaged companions at 4-5 micron, we are conducting the MIRACLES survey with VLT/NACO to systematically complement the SEDs of ~15 objects with Brackett-alpha (4.05 Tomas Stolker micron) and M' (4.8 micron) photometry. I will describe the challenges of observing at thermal (ETH Zurich) wavelengths and how the data is processed and analyzed with PynPoint (a publicly-available, generic, end-to-end pipeline for high-contrast imaging data), including a robust extraction of a companion's flux and uncertainty. Then, I will briefly introduce species, which is a new toolkit for analyzing spectral and photometric data of planetary and substellar atmospheres. We have compared the fluxes and colors of our sample with older field dwarfs, other directly imaged objects, and evolutionary models, with the aim to find trends related to spectral type and surface gravity. Finally, I will highlight the predictions by various atmospheric models in this wavelength range and show how the photometric characteristics can be affected by clouds and chemical composition. P1-13 Searching for Of all the planetary systems that have been directly imaged, HR 8799 is the best studied. Additional Outer Though four gas giants have been discovered out to a radius of 68 AU, the system is known to Planets Around host a large debris disk beginning at approximately 145 AU. It is therefore worth searching for HR8799 additional companions beyond the orbit of the furthest known planet, but none have so far been detected. In this work, we reduce the deepest integration yet of the system at L’ and large separations using a new optimized LOCI pipeline and set strong upper limits on the existence of William Raal Thompson large planets out to a radius of 250 AU. This non-detection has implications for the study of (University of Victoria) debris disks and planet formation.

P1-14 First Constraints on the Studying 3D architectures of planetary systems presents a unique window into their formation 3D Angular histories. A full description of a system’s geometric orientation requires measuring the stellar Momentum spin, planetary spin, and orbital angular momentum vectors. In the past, studies have focused on Architecture of a just one or two of these vectors, namely the orbital plane and the stellar spin axis. For instance, Planetary System measurements of projected spin-orbit alignment have found a number of hot Jupiter systems that are misaligned, raising the possibility that the misalignments resulted from high- eccentricity migration and dynamical interactions between planets. In addition, while Marta Levesque Bryan discoveries of multi-planet compact coplanar systems indicate smooth disk migration, a handful (UC Berkeley) of these systems exhibit spin-orbit misalignment, suggesting the disk itself was tilted relative to the stellar spin axis. While these partial views of 3D architectures provide an important

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perspective on planet formation, we can learn even more about system formation histories by characterizing all three angular momentum vectors. Here we present our study of the directly imaged single-planet system 2M0122-2439, the first to characterize all three angular momentum vectors of a planetary system. In this study we measure for the first time projected spins for both star and planet from our NIR high-resolution Keck/NIRSPEC spectra. We combine these with our new stellar photometric rotation period measurement from TESS data and with a previously published planetary rotation period to obtain spin axis inclinations for both objects. We fit multiple astrometry epochs, including two unpublished epochs, to constrain the companion’s orbital inclination. With these pieces needed to measure the three angular momentum vectors, we provide first measurements of the planetary obliquity, stellar obliquity, and relative inclinations between star/planet spin axes, allowing us to place new constraints on this system’s formation history. P1-15 Unveiling a population We present new results concerning the binary fraction of low mass stars in young clusters. This of sub-stellar binary work is based on HST WFC3 observations of low mass stars in the Orion Nebula Cluster. companions in a young We start from a catalog of ~1500 targets classified as bona-fide cluster members, based on a cluster: HST survey of color diagnostics relying on the presence of atmospheric water vapor, and we perform PSF the Orion Nebula subtraction on each source to search for close companions within 0.8 arcsec, or approximately Cluster in the H2O 1.4 310 AU projected separation. We discover a sample of 70 cluster candidate binary systems; of µm absorption band them, 53 were never detected before and 7 of them are compatible with planetary-mass companions. Based on a statistical model of the ONC, we estimate that at most 10% of these detections can be explained by chance alignment: the majority of our sample consists of Giovanni Maria physically associated pairs. Strampelli The sheer number of detections allows us to obtain an unprecedented statistical snapshot of (STScI) young planetary- and brown dwarf-mass companions in Orion. Our value for the binary fraction of the cluster is 14.6 % ± 1.0%, about 1.6 times higher than previous estimates. We study the mass distribution function for the primaries and companions finding a sharper peak at ~0.1 for the companion mass function vs. a relatively broad maximum for the primaries. We analyze ⨀ the mass ratio distribution of our sample, finding a bottom-heavy distribution with a median𝑀𝑀 value ~0.35: [Mc/Mp]. Finding spectroscopic signatures of low-mass stars and their companions will become even more efficient with the launch of the infrared-sensitive JWST. NIRCam imaging, in particular, will increase drastically the number of targets and enable astrometric monitoring campaigns to confirm which pairs are chance alignments and which are physically associated. P1-16 The new COPAINS tool We present COPAINS (Code for Orbital Parametrisation of Astrometrically Inferred New for target selection and Systems), an innovative tool developed to identify new directly-imaged companions based on orbital characterisation changes in stellar proper motions. Our procedure allows for the computation of masses and of direct imaging separations of hidden companions compatible with observed astrometric trends, providing a systems good indication of the region of the parameter space where invisible secondaries may be located. This in turn enables us to robustly select the most promising targets for direct imaging campaigns. Such an informed selection method promises to reduce the null detection rates from Clemence Fontanive current programs. For systems identified via this method, a second functionality of the (University of Bern) COPAINS tool then allows us to strongly characterise the orbit of newly-discovered companions using very limited orbital coverage from imaging observations. The calculation of dynamical masses for astrometric companions with minimal observational data offers a powerful way to circumvent the large uncertainties introduced by theoretical models in the substellar regime. Obtaining larger samples of model-independent masses for such benchmark objects will be crucial to calibrate and refine evolutionary, atmospheric and formation models for brown dwarfs and giant exoplanets. P1-17 Detecting distant, sub- Modeling of the gap structures in protoplanetary disks revealed by the Atacama Large Jovian planets in Millimeter Array suggests that sub-Jupiter-mass planets may be common at large orbital scattered light through separations. If true, this imposes fundamental constraints on theories of planet formation to both their circumplanetary form giant planet cores quickly at large orbital separations, and to sufficiently suppress runaway debris disks gas accretion to yield the inferred planet mass function. Unfortunately, while future direct imaging instruments will push toward detecting ever-smaller planets closer to their host star, directly imaging this putative population of distant sub-Jupiters at typical contrast ratios of 10-10 Daniel Tamayo - 10-12 in the near infrared will remain out of reach for the foreseeable future. (Princeton University) However, building on models of circumplanetary debris disks (CPDDs) by Kennedy & Wyatt (2011), we show that debris from collisions between irregular satellites can increase young planets’contrast ratios by orders of magnitude. Dozens of irregular satellites are found around

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each of our own giant planets, and represent the most collisionally evolved population in the solar system, betraying bright CPDDs in the past. We find that exoplanetary CPDDs would have been below the GPIES survey’s detection threshold. However, depending on irregular satellites' capture mechanism and efficiency, we show that by optimizing the target selection for finding such structures, the CPDDs of this population of long-period, Neptune-mass planets may be detectable with current instrumentation, and with contrast ratios between 10-8 and 10-5 over a wide range of parameter space, demonstrate that it should be an important science case for the next generation of direct imaging with ELTs and WFIRST coronography. We argue that such structures can be unambiguously identified through their strong polarization signatures and discuss their implications for our understanding of not only planet formation but also our own Solar System’s history. P1-18 Imaging Temperate While the current population of directly imaged planets is relatively hot, most exoplanets are Exoplanets older and cooler. 8-meter telescopes are sensitive enough to detect a handful of temperate (300K) planets with thermal infrared imaging and integral field spectroscopy. The ELTs will be sensitive enough to detect hundreds if not thousands of temperate exoplanets. I will present Andy Skemer simulations of different populations and science cases enabled by thermal imaging of temperate (UC Santa Cruz) exoplanets. As a demonstration of the characterization science, I will present the first thermal infrared spectroscopic sequence of brown dwarfs ranging from 500 K down to 250 K. P1-19 High Spatial Resolution The Arizona Lenslets for Exoplanet Spectroscopy (ALES) mode of the Large Binocular Thermal Infrared Telescope Interferometer is the first adaptive-optics-fed integral field spectrograph capable of Integral Field delivering 3-5 micron spectral data cubes of directly imaged exoplanets and substellar Spectroscopy companions. By extending spectroscopic wavelength coverage of the spectral energy distributions of companions beyond near-infrared spectrophotometry, we become more sensitive to the ensemble of atmospheric processes that shape their thermal emission. ALES Zackery Wyatt exists as a precursor instrument to the proposed third generation Keck instrument, SCALES, Briesemeister and the red channel of the proposed second generation TMT instrument, PSI. Through detailed (University of California, instrument simulation, we evaluate the sensitivity of the integral field spectrograph modes of the Santa Cruz) three instruments for LBTI, Keck, and TMT, respectively, for various science cases.

P1-20 Active minimization of An issue in long-exposure high-contrast images is the stellar speckle residue owning to the non- non-common path common path aberrations (NCPA) between the adaptive optics (AO) sensing and the aberrations using a self- coronagraphic science imaging channel. Observing strategies like angular/spectral differential coherent camera for imaging can calibrate a posteriori the speckle pattern whose evolution lifetime is larger than the imaging exoplanetary time required to acquire a complete sequence of images (typically 30min-1h). However, NCPA systems. that evolve during science acquisition cannot be calibrated correctly and limit the detection level creating evolving speckles in the coronagraphic images. It is thus an essential requirement to correct these speckles as they are well known to imitate exoplanets. Garima Singh The self-coherent camera (SCC), a focal plane sensor, is a tool specifically designed to (LESIA, Observatory of adaptively estimate the aberrations directly from the science image. The stellar speckle intensity Paris) can be minimized in a specified dark hole (DH) by commanding a deformable mirror. On the THD2 bench at LESIA at Observatoire de Paris, a DH with a contrast of <1e-08 between 5-12 λ/D at 785nm can be achieved routinely with the SCC under space simulating conditions. To characterize the performance of SCC under the ground-based conditions, we have installed a rotating phase screen that optically simulate the residual aberrations behind the SPHERE/VLT AO system. In preliminary laboratory results, we recorded long-exposure coronagraphic images simulating the evolving SPHERE AO residuals. Quasi-static aberrations evolving on the scales of a few exposures are actively corrected by the SCC. We created a DH with a 1-sigma contrast of <1e-06 between 5-12 λ/D (783nm) in images recorded with exposure time corresponding to 18s at VLT. In my presentation, I will remind the principle of the SCC and present the results obtained in laboratory. I will explain the future study envisioned including the possible implementation to existing instrument like SPHERE/VLT or to future instruments like PCS/ELT. P1-21 RSM detection map for Beyond the choice of wavefront control systems or coronographs, advanced data processing direct exoplanet methods play a crucial role in disentangling potential planetary signals from bright quasi-static detection in ADI speckles. Among these methods, angular differential imaging (ADI) for data-sets obtained in sequences pupil tracking mode (ADI sequences) is one of the foremost, considering the many observing programs performed with ADI-based techniques and the associated discoveries. Inspired by the field of econometrics, we propose in this paper a new detection algorithm for ADI data sets, Carl-Henrik Dahlqvist deriving from the regime-switching model first proposed by Hamilton (1988). The proposed

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(ULiege (STAR)) model is very versatile as it allows the use of PSF-subtracted data sets (residual cubes) provided by various ADI-based techniques, separately or together to provide a single detection map. The temporal structure of the residual cubes is used for the detection as the model is fed with concatenated series of pixel-wise time sequence. The algorithm provides a detection probability map by considering for concentric annuli two possible regimes, the first one accounting for residual noise and the second one for planetary signal. The algorithm performance is tested on a couple of data sets from VLT/NACO and VLT/SPHERE. The results show an overall improvement in the receiver operating characteristic space when compared with several state- of-the-art ADI-based post-processing algorithms. P1-22 Deformable Mirrors Deformable Mirrors are used in coronagraph instruments operating in ground and space-based Controller observatories. However, the requirements are different for each case. Ground-based Architectures for High- coronagraphs need to cancel atmospheric turbulence at high speed and quasi static speckles Contrast Imaging created by optics aberrations. Thus, the stroke required is larger than 1 micron and control Overview speeds need to be faster than 1KHz. In contrast, for space-based observatories, stroke and speed are not important. But, resolution and stability are the critical parameters. Moreover, for space applications, volume, mass and power consumption are tightly constrained. Eduardo Bendek In this paper, we review the state of the art of two different deformable mirror controller (NASA Jet Propulsion architectures. One is a multiplexed approach using Switch-Mode Application Specific Laboratory) Integrated Circuit (SM-ASIC). A 32x32 format SM-ASIC has been successfully prototyped and is undergoing environmental testing. This SM-ASIC is designed with ultralow static power dissipation, such that an entire ASIC consumes only ~2mW static power. This is an improvement of two orders of magnitude in static power compared to that of traditional driver electronics. The second one is the hybrid ISIC in which high-voltage Digital Analog Converters are utilized in parallel to drive the total number of actuators simultaneously. This approach, aims to bridge the gap between current bulky electronics and future single-chip ISIC DM driver controller with a solution that is commercially available now. This concept was pioneered at NASA Ames with the development of a Miniaturized DM controller for the BMC Kilo DM. This device features 1024 channels with 16bits dynamic range. It fits in a 1U cubesat volume, weight less than 1 kg, and consumes less than 10W. Several units are in operation at the NASA Ames ACE coronagraph testbed, Picture-C coronagraph, and at JPL’s HCIT. © California Institute of Technology 2018. All rights reserved. Government sponsorship acknowledged. P1-23 How to speed up your The search for exoplanets and the characterization of their atmospheres required high-contrast simulations of ground- imaging (HCI) instruments to detect objects orbiting at small angular separations from their host based images stars. For ground-based observations, such instruments rely on the adaptive optics (AO) technology to correct the effects of Earth atmospheric turbulence. Simulation of HCI behind ground-based telescopes is necessary to predict their performance and optimize their designs. Lucie Yvette Claudine One needs for example to numerically simulate images recorded for a given exposure time to Leboulleux evaluate the quality of the image (photon noise level, impact of optical aberrations and of AO (LESIA, Observatoire de residuals, etc.). Nowadays simulating one long exposure image means drawing several Paris-Meudon) thousands of random phase screens, simulating the image associated with each of them, and averaging all the images. Such a process is time consuming and demands lots of computer resources. To tackle this challenge, we developed an analytical model to directly express the ground-based AO-corrected images for finite exposure times. This model requires only the statistical properties of the atmospheric turbulence and a few random drawing for each simulated long exposure. The computation time is thus drastically decreased and such a model will allow to explore a larger range of parameters for the optimization of future instruments such as the planetary camera and spectrograph (PCS) of the ELT or SPHERE+ for the VLT. In our presentation, we will discuss our approach and show a preliminary validation of the model in the context of a ground-based imager without coronagraph. The near future work will include the extension of this model to HCI instruments. P1-24 Generating Realistic The JWST coronagraphs will enable imaging of faint and dusty objects around central hosts Coronagraphic Images with an unprecedented combination of sensitivity and angular resolution, at wavelengths from 2 of Point Source to 23 µm. The JWST Coronagraphs Working Group at the Space Telescope Science Institute, Detections with JWST's along with the Instrument Teams and internal/external partners, work towards providing the NIRCam and MIRI community with the best possible preparation tools, documentation and pipelines. In this contribution, we use PanCAKE (a toolkit for adding advanced coronagraph simulations on top of the ETC's Pandeia engine), as well as ramp simulators, to generate pipeline-compatible data Julien H. Girard and to showcase the capabilities of NIRCam and MIRI to recover known companions at high

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(Space Telescope contrasts and short separations. We aim at comparing our results with other tools available to Science Institute the community, as well as generating reliable coronagraphic images to prepare for (STScI)) commissioning activities. P1-25 Searching for Alpha The James Webb Space Telescope (JWST) will be the first space-based observatory equipped Centauri A with an mid-infrared coronagraph. JWST’s MIRI instrument offers a coronagraphic mode using Companions with the a four-quadrant phase mask (4QPM) with the sensitivity needed to resolve circumstellar James Webb Space companions at 1” at levels of raw contrast of ~10-5 (5-sigma). Here we examine the prospects Telescope MIRI for observing alpha Centauri A with MIRI, our closest solar-type neighbor, to search for Coronagraphic Mode exoplanets at separations of 1-2 AU. We generate MIRI images with the MIRI-ImSim, and reduce the raw products of the observation with a state-of-the-art data reduction technique based on principal component analysis. Our simulations include telescope aberrations, thermal Jorge Llop Sayson induced wavefront error drifts, and detector noise. Our simulations show that a carefully (Caltech) planned observation strategy would have the sensitivity to detect 0.5 RJup planets with an on- target integration time of 3.5 hours. An exo-zodiacal cloud only a few times brighter than our own should also be detectable. Moreover, these observations would push the limit of the JWST coronagraphic capabilities, and will thus offer an example of the challenges of space coronagraphy in general. P1-26 The WFIRST WFIRST is a 2.4-m telescope with an obscured pupil and two instruments: a wide-field imager Coronagraph telescope (WFI) and a coronagraph (CGI). The CGI is a technology development instrument intended to simulator: Building a advance high-performance, space-based direct imaging of exoplanets. coronagraph calibrator After the CGI is assembled and aligned, it will be tested in air and in vacuum before integrating it with the WFIRST telescope. The validation and verification of the CGI performance requires a light source that mimics the real telescope and the stellar source. Thus, we call this source the Camilo Mejia Prada Optical Telescope Assembly simulator (OTA-s). The OTA-s illuminates the entrance pupil of (NASA Jet Propulsion the CGI, which is located on the surface of the CGI Field Steering Mirror (FSM). Laboratory) To verify the CGI performance and functionality, the OTA-s should be more stable than the coronagraph itself. Thus, imposing better than 250pm wave front stability and pupil shear of less than 0.4um. In addition, the OTA-s, should be able to inject perturbations, such as tip/tilt jitter up to 400Hz and add phase screen that inject a Wave Front Error (WFE) pattern statistically representative of the actual telescope WFE. In this paper, we discuss the design and performance of the OTA-s, as well as explain its implementation for verification and validation of CGI. The lessons learned from the development of this system will be essential to develop more advanced calibrators for HabEx and LUVOIR coronagraphs. © California Institute of Technology 2018. All rights reserved. Government sponsorship acknowledged. P1-27 WFIRST Coronagraph The Coronagraph Instrument (CGI) is one of the instruments on WFIRST that will be used to Exoplanet Scene detect exoplanets. To help plan the operation of CGI, the WFIRST Exoplanet Imaging Data Simulations Challenge seeks to expose scientists to realistic simulations of coronagraph data scenes. While the simulated data includes Hybrid-Lyot Coronagraph (HLC) and Starshade observations, we will focus on the construction of HLC scene simulations with an emphasis on the exozodiacal Junellie Gonzalez-Quiles debris disk models. We use ZODIPIC and dustmap to produce scattered light images of (SURA/NASA GSFC) exozodiacal debris for a specific planet configuration. The package dustmap in particular allows us to model debris structures in resonance with the planet(s). The exoplanet system is modeled with Lambertian scattering spheres on Keplerian orbits. We include realistic time-varying speckles and pointing errors based on integrated observatory modeling, as well as detector noise. We aim to learn new data analysis techniques from the community in order to maximize the scientific return of the WFIRST Coronagraph Instrument.

Exoplanet Theory No. Title Abstract Time Name (Affiliation) P2-01 Theoretical modeling of The hydrogen line Hα is known as an indicator of gas accretion. Recent high-contrast imaging Hα spectral profile with observations detected Hα photon in the gaseous protoplanetary disk. The Hα source is thought 1D-radiation- to be growing protoplanets embedded in the disk. More recently, at the protoplanets PDS70b hydrodynamic and c, the MUSE/VLT instrument gave us the spectral profile besides intensity of the Hα. simulation: The significant and observable Hα emission requires gas as hot as tens of thousands of Kelvin. constraining the When the gas accreting towards the protoplanets passes through strong shock-wave at the accretion rate and mass protoplanetary surface, the shock converts the mechanical energy of the accreting flow into

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of the protoplanets thermal energy and can achieve such a hot gas just after the shock. To reproduce and interpret PDS70b and c the observed Hα from protoplanets, we developed a 1D-radiative-hydrodynamic model of the shock-heated gas, which can predict the Hα line profile (Aoyama, Ikoma, and Tanigawa 2018). Here, applying the model to the accreting protoplanets PDS70b and c, we constrain the mass Yuhiko Aoyama and mass accretion rate of the PDS 70b and c with the observed profile and luminosity of the (Tsinghua University) Hα line.

P2-02 Formation of Planetary There are more than 4000 exoplanets have been observed up to now and hundreds of multiple Systems in Mean planetary systems among them. Many planet pairs are in the configuration of mean motion Motion Resonances resonances (MMRs) or near MMRs. We propose a formation scenario for the planetary configurations near 3:2 and 2:1 MMRs. Firstly, the low-mass planets form at a distant region rather than at their present locations; then they will undergo type I migration until they reach the SU WANG inner region of the gaseous disk and stop migrating. Subsequently, tidal interactions between (Purple Mountain the planets and the central star will circularize their resultant orbits. Based on this formation Observatory) scenario, we find that (1) The KOI-152 system can form follow this scenario and planets may form at the late stage of star evolution; (2) the proportions near 1.5 and 2.0 can reach 14.5% and 26.0%, which are consistent with the observation data; (3) mass accretion process of planets will affect the final configuration of systems; (4) giant planets can also involve into near mean motion resonances configurations; (5) the profile of gas disk in one important factor which will lead to the near mean motion resonance configuration.

Disk Imaging No. Title Abstract Time Name (Affiliation) P3-01 Water ice mapping Water ice grains in the protoplanetary disk are believed to play an important role on the planet toward protoplanetary formation, although their spatial distribution is not well constrained with the observations. We disk have been trying to derive the water ice distribution in the disk using 3um water ice absorption mapping of the disk scattered light. Mitsuhiko Honda In this presentation, we will show our observational trials so far, and future prospects on this (Okayama University of science topic with the future facilities such as TMT/MICHI and others. Science) P3-02 Subaru Telescope Currently more than 150 planets have ever been discovered in binary or multiple systems. It is High-contrast also known that stars tend to form in binary or multiple systems, which indicates that many Observations of disks in planets would form in environments of binary or multiple systems. Therefore, to understand multiple systems planet formation, it is quite necessary to investigate planet formation processes in binary systems. Undoubtedly, to understand their formation process, not only theoretical work but also direct observations towards the protoplanetary disks in young binary/multiple star systems is Yi Yang quite necessary. By doing high-contrast polarimetry observations with the instrument HiCIAO (National Astronomical mounted on the 8.2-m Subaru Telescope in Hawaii, the complicated structures around the Observatory of Japan) young binary GG Tau A, T Tau and FS Tau are successfully resolved. We analyzed the resolved structures such as circumbinary ring, the gap opened by the binaries, and the streamer triggered by the binaries, and discussed the disk-binary misalignment based on our results. These results will be quite beneficial for us to improve current theories of disk evolution as well as planet formation process in binary systems. P3-03 New constraints on the We search a large parameter space of the LkCa 15's disk density profile to fit its observed radial dust and gas intensity profile of 12CO (J = 3-2) obtained from ALMA. The best-fit model within the distribution in the parameter space has a disk mass of 0.1 Solar mass, an inner cavity of 45 AU in radius, an outer LkCa 15 disk edge at ~ 600 AU, and a disk surface density profile follows a power-law of the form of r-4. The dust continuum map at 0.87 mm of the LkCa 15 disk shows an inner cavity of the similar size of Sheng Jin the best-fit gas model, but its out edge is at ~ 200 AU, much smaller than the fitted gas disk. (Purple Mountain Observatory) P3-04 Structure of the Recent ALMA observations have found that detailed structures are formed in protoplanetary protoplanetary disk disks. Understanding the structure of protoplanetary disks is important for revealing the around V1094 Sco environment of planet formation. In this work, we investigate the structure of the protoplanetary obtained from dust disk around V1094 Sco. The previous study indicates that the disk around V1094 Sco is cold continuum emission and massive according to its spectral energy distribution (Tsukagoshi et al. 2011). Moreover, and SED ALMA observations at Band 6 and 7 found that two ring structures are formed in the disk (van Terwisga et al. 2018). To understand the physical nature of the disk, we investigated its

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temperature and surface density distributions using our ALMA observation data of dust Sanemichi Z. Takahashi continuum at Band 8 and SED, and compared them with the radiative transfer calculations. (NAOJ) According to the dust continuum emission at Band 8, we found that the disk consists of two regions, inner bright region (< 100 au) and outer dark plateau (> 100 au), in which the radial profile of the intensity is shallower than the inner bright region. Our radiative transfer calculations indicate that the inner region is optically thick and the outer plateau is optically thin. The radiative transfer calculations also suggest that the small grains are depleted in the disk to reproduce SED. We also found that the radiative transfer calculations can reproduce the small excess in ~ 30 um of SED well when the disk inner edge is puffed up. P3-05 Investigating the gas- We present ALMA observations of the 99 GHz dust continuum and the to-dust ratio in the 13CO J = 1 - 0 and C18O J = 1 - 0 line emissions of the protoplanetary protoplanetary disk of disk associated with HD 142527. The 99 GHz continuum shows a strong HD 142527 azimuthal-asymmetric distribution similar to that of the

previously reported 336 GHz continuum, with a peak emission in dust

Munetake Momose concentrated region in the north. The disk is optically thin in both (Ibaraki University) the 99GHz dust continuum and the C18O J =1−0 emissions. We derive the distributions of gas surface density, dust surface density, and the spectral opacity index of dust grains (β) in the disk from ALMA Band 3 and Band 7 data. The G/D varies azimuthally with a relation G/D -0.53 Σg , and the β-index is derived to be 1 and 1.7 in the northern and southern regions of the disk, respectively. These results are consistent with the accumulation of larger dust grains in ∝a higher pressure region. In addition, our ≈results show≈ that the peak of dust surface density is located ahead of the peak gas surface density. If the latter corresponds to a vortex of high gas pressure, the results indicate that the dust is trapped ahead of the vortex, as predicted by some theoretical studies. P3-06 ALMA reveals a 2MASS J16042165-2130284 hosts a nearly face-on pre-transitional disk, known by a large disk misaligned, HCO+-rich, plus a cavity ~60 au in radius with symmetrical dips seen in scattered light imaging. Such inner gas disk inside features are just starting to be discovered in disks. To investigate the kinematic structure and the large cavity of the spatial distribution of gas and dust in this uniquely interesting disk, we carried out 0''.2 transitional disk resolution Atacama Large Millimeter/submillimeter Array imaging in continuum, CO (3-2) and around J160421.7- HCO+ (4-3) in Band 7 (0.87 mm) (Mayama et al. 2018, ApJL, 863, L3). Where continuum 213028 image showed a seemingly empty cavity, HCO+ (4-3) allowed us to reveal a central component detected at 12σ. Spectral resolution allowed us to peer into the kinematical structure of the disk, including the unresolved central component. It shows a stark difference in the kinematics Satoshi MAYAMA between the outer and the inner disk, manifested as a 35° misalignment in the observed position (SOKENDAI(The angle. A twisted butterfly pattern is found in the moment 1 map of CO (3-2) emission line Graduate University for towards the center, which is the key signature of a high misalignment between the inner and Advanced Studies)) outer disks. In addition, the counterparts of the shadows are seen in both dust continuum emission and gas emission maps, consistent with these regions being cooler than their surroundings. Our findings strongly support the hypothesized misaligned-inner-disk origin of the shadows in the J1604-2130 disk. Finally, by comparisons with recently published VLT monitor imaging results, we discuss the possibility that its internal asymmetric structures cause the variations on the light curve of the host star. P3-07 The derivation of the Analyzing multiband observations of dust continuum emission is one of the useful tools to dust properties using constrain dust properties which help us to understand the physical properties of the disks. We the synthetic ALMA perform the synthetic ALMA multiband analysis to find the best ALMA band set for multiband analysis constraining the dust properties of the TW Hya protoplanetary disk. We find that the Band [10,6,3] set is the best set among the possible combinations of ALMA Band [3,4,5,6,7,8,9,10]. We also find two conditions for the good ALMA band sets providing narrow constraint ranges Seongjoong Kim on dust properties; (1) Band 9 or 10 is included in the band set and (2) Enough frequency (Tokyo Institute of intervals between the bands. These are related with the conditions which give good constraints Technology) on dust properties: the combination of optically thick and thin bands are required, and large β (β is the power-law index of dust opacity, κν νβ) and low dust temperature are preferable. To examine our synthetic analysis results, we apply the multiband analysis to ALMA archival data of the TW Hya disk at Band 4, 6, 7, and 9. ∝Band [9,6,4] set provides the dust properties close to the model profile, while Band [7,6,4] set gives the dust properties deviating from the model at all radii with too broad constraint range to specify the accurate values of dust temperature,

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optical depth, and β. Since these features are expected by the synthetic multiband analysis, we confirm that the synthetic multiband analysis is well consistent with the results derived from real data. P3-08 The detection of a dust We report the observations of the dust continuum at 225 GHz and CO ring beyond the outer isotopologue (12CO, 13CO, and C18O) J = 2−1 emission lines toward the edge of the dust disk protoplanetary disk around CR Cha using the Atacama Large around CR Cha Millimeter and Submillimeter Array (ALMA). Dust continuum image is

obtained with a high angular resolution of 0.1′′, which shows a deep and Seongjoong Kim wide gap at the disk radius of 90 au with the depth of 34% and the width of 10 au. A faint dust ∼ (Tokyo Institute of ring is located around 120 au, beyond the outer edge of the dust disk. The dust continuum and Technology) CO line images show that the size of the gaseous disk is larger than that of the dust disk. The line ratios between the CO isotopologue emissions show that the 12CO and 13CO lines are optically thick. The radial profile of the peak brightness temperature of the 13CO line shows a bump at 130 au. We investigate two possible mechanisms for reproducing the observed dust gap, ring, and a bump of 13CO line. First, the observed gap structure can be interpreted to be opened by a sub-Jupiter mass planet. Meanwhile, the radiative transfer calculations using the dust surface density profile obtained from our observations show that the observed dust ring could be caused by dust accumulation at the gas temperature bump, that is, the gas pressure bump produced beyond the outer edge of the dust disk. P3-09 Discovery of an The gas-rich debris disk of HD 141569, first discovered in 1999 with the HST in near-IR and azimuthal density later in visible revealed structures such as multiple rings and outer spirals extended as far out as gradient in a gas-rich ~410 AU. More recently, the direct imaging SPHERE instrument has resolved several non- debris disk possibly uniform concentric rings inside the inner cavity (<100 AU) in near-IR. A North-South related to a massive asymmetry was discovered in the brightest and innermost ringlets at 40 AU, which is aligned collision with the disk projected major axis. This observed asymmetry cannot be explained by the light scattering properties of dust. We proposed instead an azimuthal variation of the dust density. However, this interpretation is complicated by the post-processing techniques commonly used Garima Singh for scattered light disk observations in total intensity, which particularly impact the shape and (Observatory of Paris) local photometry of extended objects. In 2017, we have acquired polarimetric data using the dual polarimetric imaging mode of SPHERE/IRDIS. We discovered that the Lorentzian azimuthal distribution of the intensity reported in the innermost ring in Perrot et al. (2016) is significantly different in total intensity and polarized intensity. Assuming a model based on the massive collisions between planet embryos, we found that both images can be described as a combination of a phase function and an azimuthal density variation which takes a Lorentzian profile peaking to the south-west of the ring. The complementarity of polarimetric and total intensity images has allowed us to constrain the actual dust density distribution and to relate this morphology to a potential massive collision. In this talk, I will introduce HD141569 followed by the imaging modes of SPHERE and the disk structure observed within 100 AU both in total and polarimetric intensity. I will then present the hypothesis that observed asymmetries are produced by an azimuthal variation of the dust density, possibly connected to massive collisions. P3-10 First resolved Direct imaging of debris discs gives important information about their nature, their global observations of a highly morphology, and allows us to identify specific structures possibly in connection with the asymmetric debris disc presence of gravitational perturbers. It is the most straightforward technique to observe around HD 160305 with planetary systems as a whole. We present the first resolved images of the debris disc around the VLT/SPHERE young F-type star HD 160305, detected in scattered light using the VLT/SPHERE instrument in the near infrared. We used a post-processing method based on angular differential imaging and synthetic images of debris discs produced with a disc modelling code (GRaTer) to constrain the Clement Perrot main characteristics of the disc around HD 160305. All of the point sources in the field of the (Universidad de IRDIS camera were analysed with an astrometric tool to determine whether they are bound Valparaiso, NPF, objects or background stars. LESIA) We detect a very inclined ( 82°) ring-like debris disc located at a stellocentric distance of about 86 au (deprojected width 27 au). The disc displays a brightness asymmetry between the two sides of the major axis, as can be expected from scattering properties of dust grains. We derive an anisotropic scattering factor g>0.5. A second right-left asymmetry is also observed with respect to the minor axis. We measure a surface brightness ratio of 0.73 ± 0.18 between the bright and the faint sides. Because of the low signal-to-noise ratio (S/N) of the images we cannot easily discriminate between several possible explanations for this left-right asymmetry,

41 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

such as perturbations by an unseen planet, the aftermath of the breakup of a massive planetesimal, or the pericenter glow effect due to an eccentric ring. P3-11 First detection of a very HD121617 is a 16 Myr old debris disc discovered thanks to the detection of an infrared excess sharp ring in near- in the spectral energy distribution with AKARI. Also it host a ring of gas which have been infrared light with detected by ALMA. We present the first resolved observation of a dust ring in near-infrared VLT/SPHERE around light with SPHERE around this star. The detected dust disc present a very light eccentricity and HD 121617. the surface density of the inner edge is very sharp. It may be the consequence of the gravitational interaction with a massive companion. We also shown that the dust ring is localized at the same place that the gas ring, which ask the question of the gas origin. At 16 Myr Clement Perrot the detected gas should be a second generation gas because the primordial gas should have (Universidad de disappeared already. To understand the morphology of the dust ring and the origin of the gas we Valparaiso, NPF, performed 2D hydrodynamical simulations, using a set of planetary mass and position. LESIA) P3-12 SPHERE Observations We present the first detection of scattered light from the hot dust around the nearby star HD of Debris Disks 172555 and the new observations of debris disks around HD 15115 and HIP 79977 with SPHERE (Spectro-Polarimetric High-contrast Exoplanet REsearch) at VLT. HD 172555 is a ~23 Myr A7V star at a distance of 28.6 pc. The spectral energy distribution of the disk shows a Natalia Engler very pronounced silicate feature at 9.8 micron implying the presence of a large amount of (ETH Zurich Institut for micron-sized "hot" dust grains. Using the polarimetric differential imaging technique with Particle Physics and ZIMPOL (Zurich IMaging POLarimeter), we obtained high-contrast images of the debris disk Astrophysics) with a spatial resolution of ~25 mas and an inner working angle of ~0.1 arcsec. By fitting a model of the spatial distribution of dust grains to these images, we find that the disk has a radius of 0.30- 0.35 arcsec (~10 au) and an inclination of ~105 degrees. Our new high-contrast and high- resolution images of the debris disk "Blue needle" (HD 15115, a 25-100 Myr F4IV star at a distance of 48.2 pc) and HIP 79977 (a 15 Myr F2/3V star at a distance of 123 pc) in scattered (total intensity) and in polarized light provide a much clearer view of the disk structures and their asymmetries. P3-13 Dust production in Optical and near-infrared observations at high angular resolution reveal the population of small young debris disks dust grains in debris disks. Those small second-generation dust grains must originate from collisions of larger bodies in the so-called “birth ring”. Most of those grains feel the radiation pressure from the central star and as a consequence their orbit will spread farther out from the Johan Olofsson birth ring. By studying the radial and azimuthal distribution of those dust grains one can better (Instituto de Fisica y characterize how and where the dust is being produced. I will present our modeling effort of Astronomia, Valparaiso) SPHERE/ZIMPOL observations of the disk around HR 4796 and will describe our model that can self-consistently reproduce almost all the available observations (SPHERE, ALMA, and mid-infrared data, only recently published HST observations proved challenging to be modeled). I will discuss possible scenarios that can explain the observed morphology (e.g., brightness asymmetry) of this very interesting bright debris disk. P3-14 The Surprising HR 4796 A is a close-by young A0 star. Its narrow and sharply carved belt debris disk made it a Scattering Phase very popular target for all imaging instruments from the visible to the far IR since then, Function of HR 4796 A constraining further its geometrical parameters and spatial extension. Measurements of scattered light phase functions have long been used as a powerful tool to measure dust grain properties of comets and asteroids in the solar system. The total intensity, Johan Mazoyer polarized intensity, and color of the scattered light have been used to effectively constrain (Jet Propulsion particle shape, size, composition and porosity. For debris disks, high- contrast imaging Laboratory, California observations in visible and near-IR is the only method allowing the measurement of these Institute of Technology) observable and have been extracted for only a handful of disks so far. The inclination and projected distance of the HR 4796 A disk provide an opportunity to measure the scattering properties of debris dust over a large range of scattering angles. However, in total intensity, the extraction of these observables is greatly complicated by the PSF subtraction techniques applied to coronagraphic images. We have obtained observations in the J-, H-, K1- and K2-bands of the debris disk around HR 4796 A with GPI and used an MCMC method to precisely extract its SPF. We also reanalyzed with the same treatment the recently published SPHERE data (Milli et al., 2017) on HR 4796. This confirmed that the scattering phase function (SPF) is different from ones not only measured on the limited sample of debris disks but also on various dust populations in the solar system, as it features an extremely forward scattering curve, a dip at scattering angles from 30° to 70° and an increase in intensity at high scattering angles. Finally, we use a radiative transfer code to constrain the dust properties for this object.

42 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

P3-15 HD 146897; An Icy We present spectroscopic and polarimetric high contrast images of the HD 146897 (HIP 79977) Debris Disk as seen by debris disk (F star in Upper Scorpius SFR) obtained in H, J and K bands with the Gemini Planet the Gemini Planet Imager (GPI) as part of a Gemini Large and Long Program. The disk is detected in six distinct Imager observing modes and is inclined ~85 degrees with polarised disk signal extending to the edge of the GPI field of view at 1.4 arcsec. These data show that the vertical extent of the disk increases with radius and confirm the previously observed east/west asymmetry. Total intensity disk Schuyler Grace Wolff images are retrieved from the spectral data using multiple PSF subtraction methods. We (Leiden Observatory) construct wavelength dependent polarization fraction scattering phase functions (SPFs) for intermediate scattering angles (20 - 90 degrees) to constrain the dust properties of the disk. We model the SPFs using radiative transfer modeling under the assumption of aggregates that can be approximated with the DHS framework. Exploration of the parameter space provides constraints on the dust composition (volume fractions for icy grains, amorphous carbon and amorphous silicates) and particle size, leading to a mostly icy composition and a shallow size distribution. P3-16 A Survey for Resolved With the high-contrast polarimetry mode of the Gemini Planet Imager (GPI), we are conducting Debris Disks in the Sco- a disk morphology survey of on a complete sample of high infrared excess A/F-stars in the Sco- Cen Association Cen OB Association regions Lower Centaurus Crux (LCC) and Upper Centaurus Lupus (UCL). Near-IR scattered-light imaging has the highest angular resolution of all techniques used for debris disk imaging. Dust belts, cleared gaps, offsets, and asymmetries can be clearly measured, Jennifer Patience allowing inferences on disk dynamics and evolution. Measurements of brightness and (Arizona State polarization fraction variations with scattering angle can be used to constrain dust grain size and University) composition, factors related to the collisional state and material makeup of the planetary system. As part of the large-scale GPI Exoplanet Survey program, a set of 18 Sco-Cen members with infrared excesses were observed, and GPI polarized light of these targets spatially resolved disks around 80per-cent of the stars, the highest detection rate of any population observed with GPI. The Sco-Cen region is also the site of several imaged planetary mass companions. Our ongoing program is designed to observe the remaining 12 highest IR excess A/F-star targets in LCC/UCL not yet observed with GPI polarimetry mode. Of the targets observed thus far, five disks have been resolved, including systems with asymmetries and with inclinations favorable to investigating a large range of scattering angles. Combining the existing and ongoing disk structure surveys of Sco-Cen, we will assemble a consistent experimental dataset to explore the diversity of disk properties around stars with a common age and formation environment. The newly revealed structures will place constraints on the disk properties and will search for dynamical signatures of disk-planet interactions. P3-17 Comparison of PSF Debris disks are critical elements of planetary systems, and spatially resolved imaging is Subtraction Algorithms important component in answering key questions of debris disk dynamics, structure, and grain on Disk Imaging Data properties. Several different image processing algorithms can be utilized to generate scattered images of debris disks at optical and IR wavelengths, however, and they have different possible biases on the resulting disk maps. One of the key issues in imaging debris disks is the treatment Justin Hom of point spread function (PSF) removal, important in resolving the structure and brightness (Arizona State levels of debris disks. There are currently two main challenges to overcome in state-of-the art University) image processing of high contrast disk data: (1) the introduction of false structural artifacts that can appear as disk gaps or embedded planets and (2) systematically depressed flux levels that prevent accurate measurements of dust properties such as polarization fraction and scattering phase function. Accurate images are necessary to characterize and constrain debris disk structure, geometry, and grain properties which are key concepts in understanding planetary system evolution. This study is a comprehensive comparison of the biases and limitations of four PSF removal algorithms. A uniform approach was applied, consisting of injecting a model- generated disk of known properties into Gemini Planet Imager (GPI) datasets of single stars and then utilizing different image processing algorithms to make a resolved disk image to be compared with the known input disk. Systematic biases of the image processing routines such as flux loss from self-subtraction and induced artifacts are quantified for each technique and for a range of disk geometries and brightness levels. In addition to the study of simulated disks, the results from a uniform analysis of the surface brightness profiles and polarization fractions of a set of bright GPI-resolved debris disks is reported. P3-18 The Eroding Disk of We report HST STIS coronagraphic imaging of the disk of AU Mic from 2017 combined with AU Mic: Implications archival data from 2010-2011. Outward motion of the features first identified in 2015 continues. for the Habitability of We find additional features in the NW arm, as well as morphological changes to the features in M-star Terrestrial the SE arm. Feature elevation changes are confirmed, but the HST data, by themselves are too Planets sparse to establish whether these show the 5-year chromospheric period or change more rapidly,

43 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

possibly due to stellar flares. By combining disk mass estimate based on ALMA data with feature mass estimates and the number of features likely reaching escape velocity within a Carol Anne Grady decade, we estimate a residual lifetime for AU Mic’s disk of only 1.35 Myr. With a current age (Eureka Scientific) of 23+/-4 Myr, the residual lifetime is consistent with the observed scarcity of debris disks around M stars by >30 Myr. This disk lifetime estimate suggests a compressed interval where minor bodies containing volatiles and organics can be perturbed into star-grazing orbits compared to the solar system. One consequence of a shortened bombardment interval is that terrestrial planets in the Habitable Zone are likely to be dry and poor in organics making them inhospitable environments for the development of surface life. P3-19 The Hunt for Using the Large Binocular Telescope Interferometer (LBTI) we have been carrying out the Observable Signatures Hunt for Observable Signatures of Terrestrial planetary Systems (HOSTS). This search for of Terrestrial planetary exozodiacal dust around nearby stars has leveraged the use of high performance adaptive optics Systems (HOSTS): and nulling interferometry to deliver critical information on the detection limits for future exo- How Much Dust should Earth imaging missions. The survey of 38 stars suggests that the median habitable zone dust We Expect in the level for sun-like stars is 4.5 [+7.3-1.5] time the solar system level. I will describe the Habitable Zone? observational results from HOSTS, as well as possible correlations with auxiliary data on these stars that can inform the distribution of dust and their parent bodies in exoplanetary systems. Phil Hinz (University of California Santa Cruz) P3-20 A high-contrast The Coronagraphic, Debris, and Exoplanet Exploring Payload (CDEEP) is a proposed low cost, SmallSat Mission SmallSat-class high-contrast circumstellar disk imager concept under active development. Concept CDEEP will survey a range of circumstellar environments, probing scattered light emission at contrasts of 10-6/as2 (10-7 per resolution element) from at visible wavelengths with a 35 cm class unobscured telescope. Such imaging will characterize the albedo and composition of disks Ewan S. Douglas previously inferred from infrared excess, test for sculpting by exoplanets, and differentiate (University of Arizona) between transport dominated and collisional disk morphologies. CDEEP is expected to provide the first resolved images of disks around dozens of stars over a 1 year mission, providing over an order of magnitude increase in contrast over the Hubble Space Telescope coronagraphs and an approximately 5x larger high-contrast outer working angle than the Wide Field Infrared Space Telescope Coronagraph Instrument (WFIRST-CGI). With an optical design optimized for coronagraphy from an ESPA Grande SmallSat, CDEEP builds on the PICTURE-C balloon heritage, including an unobscured aperture, microelectromechanical systems (MEMS) deformable mirror, and state-of-the-art vector vortex coronagraph -- which will allow imaging of warm Kuiper-belt analogs at complementary wavelengths and higher contrasts than the coronagraphs on the James Webb Space Telescope. We will present the preliminary CDEEP design and expected mission science along with future design and prototyping plans. CDEEP is a collaborative effort led by researchers at the University of Arizona with partners and collaborators at Caltech, Laboratoire d'Astrophysique de Marseille, the Massachusetts Institute of Technology, Observatoire de la Côte d’Azur, The Space Telescope Science Institute, Stanford University, and the University of Massachusetts Lowell. P3-21 SPHERE reveals Near-infrared scattered light images of protoplanetary disks frequently show evidence of warped disk around substructure like rings or shadows often attributed to misaligned inner regions. These HD 139614 misalignments can be explained, among other mechanisms, by the interactions with a misaligned companion in the disk. We observed HD 139614, a Herbig Ae/Be transition disk Gabriela Muro Aerna with a cavity of a few AU, looking for such signatures of planet-disk interactions and (University of constructed a radiative transfer model of this disk to explain the azimuthal asymmetry of the Amsterdam) outer disk. We find that a small misalignment of a few degrees of at least two inner components – the simplest approximation of a warp – is necessary to reproduce the broad shadow on this region.

Disk Theory No. Title Abstract Time Name (Affiliation) P4-01 Formation of Recent observations of protoplanetary disks with ALMA have shown that most of the observed axisymmetric disks have substructures in the spatial distribution of dust grains. In particular, multiple rings substructures via and gaps were frequently observed. These axisymmetric substructures are thought to indicate secular instabilities ongoing or completed planetesimal/planet formation. Therefore, understanding how the

44 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

triggered by dust-gas observed rings/gaps form is important to reveal the planet formation. In this work, we focus on friction and turbulent the ring/gap formation via secular instabilities, which does not require the existence of planets. viscosity in One of the secular instabilities is secular gravitational instability (GI; Takahashi & Inutsuka protoplanetary disks 2016). The secular GI grows as a result of a decrease of the Coriolis force exerted on dust due to dust-gas friction. Performing a linear stability analysis, we also find another secular instability that forms multiple rings and gaps. We call it two-component viscous GI (TVGI; Tominaga et Ryosuke T. Tominaga al. 2019). TVGI is triggered by a combination of dust-gas friction and turbulent viscosity, both (Nagoya University) of which decrease the Coriolis force and render a disk unstable. Separations of rings or gaps correspond to the most unstable wavelength, which is 3-4 times longer than the gas scale height at most. Both of those secular instabilities form rings and gaps in not only a dust disk but also a gas disk, although density contrast between adjacent rings and gaps in a gas disk is much lower than in a dust disk. We expect the present mechanism is responsible for creating multiple rings and gaps in protoplanetary disks, at least in outer regions (~100 au). We also performed numerical simulations and studied non-linear growth of the secular GI and TVGI. The results show that dust rings formed via linear growth of those instabilities collapse self-gravitationally at the non-linearly evolutionary stage, and the dust density becomes more than 10 times higher. P4-02 Clustering and collision In the standard scenario of planet formation, it is supposed that dust particles in a protoplanetary statistics of dust disk repeatedly collide and coalesce, and grow into planetesimals. However, there are unsolved particles in weakly problems on the dust growth in a turbulent protoplanetary disk, which include the radial drift, compressible bouncing, and fragmentation barriers. To solve these problems, it is important to quantitatively turbulence in understand the dynamics of dust particles regulated by a turbulent flow. protoplanetary disks According to the Minimum-mass Solar Nebula model (Hayashi 1981), the Reynolds number and the Mach number of turbulence in a protoplanetary disk range Re=108~1011 and Ma=0.01~0.32, respectively. Ishihara et al. (2018) performed direct numerical simulations Yoshiki Sakurai (DNSs) by solving the Navier-Stokes equations for incompressible turbulence at high Reynolds (Nagoya University) number up to Re = 16,100, and demonstrated that the dust growth is possible even in a strongly turbulent flow. Their results are consistent with those in weakly compressible turbulence by Pan & Padoan (2013, 2014, 2015) or Pan et al. (2014) at Ma~0.085 or 0.1. However, the effect of compressibility of protoplanetary disk turbulence on the particle statistics is not yet quantitatively investigated. In this study, we performed DNSs of forced compressible turbulence with Ma=0.1 and 0.3 and compared the results with those obtained by the DNSs of forced incompressible turbulence. As for the forcing, we conducted the cases with different ratios of dilatational and solenoidal components of the mean energy dissipation. We tracked eight sets of inertial particles with Stokes number of St=0 to 0.3 in the turbulent fields. Our results show that, depending the forcing, the compressibility can make remarkable effect on the flow field by causing density fluctuation, shocklets appearance, and reducing the enstrophy. However, we found also that the collision statistics such as particle relative velocity, collision kernel, and sticking rates are not so sensitive to the compressibility when Ma<0.3. P4-03 Dispersal of The understanding of the evolution of protoplanetary disks is crucial to understand planet Protoplanetary Disks formation processes. Although the disk evolution has been investigated considering viscous with Magnetically- accretion and photoevaporation, recently much attention has been paid to magnetically-driven driven and (MHD) winds. However, the effects of photoevaporation and MHD winds have been Photoevaporative investigated separately. Winds In this study we numerically simulate the disk evolution considering both photoevaporative and MHD winds to provide a realistic picture of disk evolution consistent with observations. We consider the photoevaporation by extreme UV and X-rays. The accretion driven by magnetic Masanobu Kunitomo braking is also considered. We found that MHD winds and photoevaporation have important (Kurume University) roles at a different situation: The former is dominant in the early phase in the inner disk, whereas the latter in the late phase in the outer disk. In particular, if we adopt the low viscous parameter, which is suggested by recent observations, the magnetic braking is required to disperse disks within several Myr. On the other hand, without photoevaporation, a low-mass disk can last even at a few tens of Myr. Therefore we conclude that both effects are needed for the disk evolution consistent with observations. P4-04 Radiation While protoplanetary disks are considered to have lifetimes of several million yr in the solar Hydrodynamics neighborhood, recent observations suggest that the disk lifetimes are shorter in low-metallicity Simulations of environments (Yasui et al. 2009, 2010). We perform a suite of radiation hydrodynamics Photoevaporating simulations of photoevaporating disks with various metallicities to study the metallicity Protoplanetary Disks dependence of mass-loss rates. Our simulations follow hydrodynamics, radiative transfer, and nonequilibrium chemistry in a self-consistent manner. We also consistently calculate dust-grain

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with Various temperatures by solving the radiative transfer of the stellar irradiation and grain (re-)emission. Metallicities As photo-heating sources for the gas, we take account of far-ultraviolet (FUV), extreme- ultraviolet (EUV), and X-ray, which have been suggested important to drive photoevaporation but either of their relative importance or their interplaying effects is not well resolved. Riouhei Nakatani In the fiducial case with solar metallicity, including the X-ray effects does not significantly (RIKEN) increase the photoevaporation rate when compared to the case with ultra-violet (UV) radiation alone. At sub-solar metallicities, the photoevaporation rate increases as metallicity decrease owing to the reduced opacity of the disk medium. The result is consistent with the observational trend that disk lifetimes are shorter in low metallicity environments. In contrast, the photoevaporation rate decreases at even lower metallicities, because dust-gas collisional cooling remains efficient compared to far UV photoelectric heating whose efficiency depends on metallicity. The net cooling in the interior of the disk suppresses the photoevaporation. However, adding X-ray radiation significantly increases the photoevaporation rate, especially at Z ~ 10-2 Zsun. Although the X-ray radiation itself does not drive strong photoevaporative flows, X-rays penetrate deep into the neutral region in the disk, increase the ionization degree there, and reduce positive charges of grains. Consequently, the effect of photoelectric heating by far UV radiation is strengthened by the X-rays and enhances the disk photoevaporation.

Instrumentation and Technology No. Title Abstract Time Name (Affiliation) P5-01 SPHERE: the current The last few years have seen a harvest of discoveries in the field of exoplanets thanks to the contrast limitations high-contrast instruments, such as SPHERE and GPI, installed on 8-m class telescopes. These instruments have been specifically designed for the detection and characterisation of exoplanets and circumstellar disks. However, by reaching a raw contrast of 1/10000 in the images, we Faustine Cantalloube landed in a regime in which higher order of aberrations become visible in the image. In this (Max Planck Institute for contribution we will highlight the contrast limitations that are currently observed with the Astronomy (MPIA)) SPHERE instrument and explain their origin, supported by simulations. We will discuss how these can be minimised in SPHERE and, by extrapolation, in future high-contrast instruments for the upcoming 40-m class telescopes such as ELT/METIS or TMT/PSI. P5-02 Prototyping High Direct imaging and spectroscopy of potentially habitable planets with ELTs will require high Contrast Imaging for contrast instrumentation significantly more sensitive and accurate than the current generation of ELTs on SCExAO: Extreme-AO systems on 10-m class telescopes. While the required performance gains can likely Users’ Guide and be achieved thanks to recent and ongoing advances in key technologies (including fast sensitive Recent Highlights detectors, high performance computing, optical coronagraphy and wavefront control), most have not yet been tested on-sky or integrated in a high contrast imaging instrument. We describe how the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system is Olivier Guyon being optimized to serve as a prototyping platform for integrating and validating these advanced (Subaru Telescope/ high contrast imaging techniques in a fully functional on-sky system. By providing a modular NAOJ, ABC & Univ. of hardware and software environment optimized for flexible prototyping, the time span from Arizona) concept formulation to on-sky operation and validation is greatly reduced. The approach also enables external research groups to deploy and test new hardware and algorithms. We highlight recent technology validation achievements and ongoing activities that are particularly relevant to the development of PSI-BLUE, the optical/nearIR arm of the Thirty Meter Telescope (TMT) Planetary System Imager (PSI) instrument. These include predictive control and sensor fusion, PSF reconstruction from AO telemetry, coronagraph development, focal plane speckle control with photon counting MKIDs cameras, and AO-enabled fiber-fed spectroscopy. We describe how ongoing upgrades to SCExAO will validate key hardware (DM, detectors) for TMT-PSI, and also how these improvements to SCExAO evolve the facility to implement the system-level architecture envisioned for the TMT-PSI instrument. P5-03 New NIR Polarimetric Young stars form in gas-rich and dusty protoplanetary disks. Direct imaging of young planetary Differential Imaging systems can reveal when, where and how the transitions from the protoplanetary disks to the Modes on the Subaru planetary systems take place. The details of planet-forming disk structures can be observed in Coronagraphic NIR polarized light. Extreme Adaptive To observe the formations and the early evolutions of planetary systems with high sensitivity, Optics Instrument we are combining high-precision NIR polarimetric differential imaging (PDI) with high-contrast imaging at the Subaru Telescope. By installing new optical components in the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system, we are developing two

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Jin Zhang complementary polarimetric imaging modes: (1) spectropolarimetric imaging with the (The University of Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) and (2) fast Tokyo) switching PDI with a high-speed low-noise NIR camera (C-RED One), both of which are unique in high-contrast imaging. The new NIR PDI modes are designed to map the planet-disk gravitational interactions, to measure the dust compositions of disks and to investigate the dust shells of evolved stars. The double-difference technique and the triple-layer differential polarization calibration will be used for obtaining the high polarimetric sensitivity to observe the inner regions of planetary systems, which are related to the formations of habitable planets. We will report the details of the new NIR PDI modes of SCExAO and the analysis of early data obtained with the new instrument. P5-04 Astrometry and Exoplanet characterization relies on extracting precision photometric (spectra, time variation) Photometry with and astrometric (orbits) measurements. In post coronagraphic images, it is challenging to Satellite Speckles measure the relative position and intensity of companion with respect to the central starlight, as it is blocked by the coronagraph. Artificial satellite spots created in post-coronagraphic images can address these issues by imprinting references in images. We demonstrate the use of a Ananya Sahoo periodic time-modulated phase grid on the Deformable Mirror of the SCExAO instrument to (Subaru Telescope, generate extremely faint satellite speckles which are incoherent with underlying speckle halo for NAOJ) calibration. We switched the grid pattern between frames to create a set of data having alternating speckle pattern. We demonstrate that by subtracting two frames with the two different speckle patterns, we remove most of the unknown background noise (speckles) which would otherwise create a bias in the photometric measurement. We report on-sky measurements of the photometric and astrometric stability of such fainter speckles over a period of 540 seconds. The effect of Strehl variation variations on measurement has been eliminated. This technique will be beneficial for characterization of directly imaged extrasolar planets and debris disks. P5-05 Overview of the SHARK-NIR is a high-contrast camera proposed in 2014 as a new generation instrument at the coronagraphic LBT. The instrument successfully passed the final design review in January 2017 and now it is capabilities of SHARK- in its AIV phase in Padova. NIR, the second- We provide here an insight on the coronagraphic capabilities of the instrument, retracing back generation high over the steps we followed to first select the techniques and then to optimize each of them contrast imager for the according to the top-level requirements and to the instrument opto-mechanical constraints. Large Binocular We also describe the end-to-end POP simulator that we developed in order to investigate the Telescope coronagraphic performance in a wide range of configurations. The simulator is able to generate sequences of coronagraphic images in presence of several sources of optical aberrations (also time-evolving). Dedicated post-processing algorithms (e.g. Angular Differential Imaging) have Daniele Vassallo been then applied to compute detection limits. We show that detection limits derived in (INAF-Osservatorio simulations for the techniques that we selected can fulfill the challenging scientific goals of the Astronomico di Padova) instrument. P5-06 XAO-assisted Several Extreme Adaptive Optics (XAO) systems dedicated to the detection and coronagraphy with characterisation of the exoplanets are currently in operation for 8–10 meter class telescopes. SHARK-NIR: from Coronagraphs are commonly used in these facilities to reject the diffracted light of an observed simulations to star and enable direct imaging and spectroscopy of its circumstellar environment. laboratory tests SHARK-NIR is a coronagraphic camera that will be implemented at the Large Binocular Telescope (LBT). After an extensive simulation campaign, SHARK-NIR team selected a suite of coronagraphic techniques to be implemented in the instrument in order to fulfil the scientific Elena Carolo requirements. (INAF – OAPd) In summary, the Gaussian Lyot coronagraph is the option to serve all those science cases requiring field-stabilization and moderate contrast. Observations in pupil-stabilized mode to search for exoplanets can take advantage of three Shaped Pupils (SP) and a Four-Quadrant Phase Mask (FQPM) coronagraph. The SP are designed for high contrast on a small field close to the star and are robust to image and pupil jitter. The FQPM allows to access the entire scientific FoV providing excellent performance in ideal conditions (high Strehl ratios), and good performance both close and further away from the star, even at lower Strehl and with moderate vibrations. After the procurement phase, the coronagraphic masks were delivered to our labs and we started to test their performance on an optical bench and define the alignment procedures that will be employed in the final integration of the instrument in our clean room. In this talk, we describe the tests that we performed in the lab with SHARK-NIR coronagraphs. We measured the contrast achievable with each technique in very-high Strehl conditions and we

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delineate the alignment and integration strategy, defining the precision of the procedures to comply with the tight alignment tolerances. P5-07 New Symmetrical A new symmetrical formulation is useful to systematically handle pupil functions and point Formulation of spread functions of hexagonally segmented telescopes (e.g. Keck, JWST, ELT, TMT, LUVOIR Hexagonally Segmented and OST). The formulation adopts two sets of three variables on pupil and image planes: (a, b, Telescopes c) = (-2α / sqrt(3), α/sqrt(3)+β, α/sqrt(3)-β) and (A, B, C) = (2β/sqrt(3), -β/sqrt(3)+ α, -β/sqrt(3)- α) on pupil planes, (q, r, s) = (-x/sqrt(3), x/(2sqrt(3))+y/2, x/(2sqrt(3))-y/2) and (Q, R, S) = (y/sqrt(3), -y/(2sqrt(3))+x/2, -y/(2sqrt(3))-x/2) on image planes, where (α, β) and (x, y) are 2-D Satoshi Itoh normalized Cartesian coordinate. Permutations of the three variables do not change the (Osaka University) expression because the formulation reflects the symmetry of the telescope apertures. Fourier transform with the formulation can be interpret as a 3-D Fourier transform of the amplitude localized onto a 2-D plane because xα+yβ = qa+rb+sc = QA+RB+SC. The PSFs of the telescopes can be written as products of square moduli of the functions that correspond to sinc function and Dirichlet kernel, which are used for 1-D segmented telescope models. The formulation enables us to classify hexagonally segmented telescopes and to label the segments with a mathematically meaningful way; therefore, only simple coding is needed to simulate the telescopes. Thus, the formulation may be helpful for coronagraphic studies aimed at the use with the hexagonally segmented telescopes. The content of this talk basically corresponds to that of Itoh S., et al. 2019, MNRAS, 483, 1, DOI: 10.1093/mnras/sty3052; but in this presentation, specific way to classify and simulate the telescopes with the formulation will be mainly focused on. P5-08 Wrapped Vortex: a The main interest of high contrast imaging instruments is the measurement of exoplanet spectra Cheap Achromatic to characterize their surface temperature and their atmosphere composition. Such instruments Coronagraph Phase need coronagraphs that attenuate the starlight over a broad spectral band. Nowadays, numerous Mask coronagraphic devices have been proposed and validated in laboratory and on-sky detecting planets that are 1e4-1e5 times fainter than their star. A few coronagraphs have been validated in laboratory attenuating the starlight by a factor of 1e8-1e10 over a broad band. Some of these use Raphael Galicher multi-stage monochromatic coronagraphs (multi-stage vortex and multi-stage four quadrant (University of Paris) phase masks) that are not easy to align and thus, that are not a good solution for a space instrument. Others are based on liquid cristal polymers. The technology is still expensive and polarization optics are needed to make them work at such contrast levels. In this presentation, we will present the wrapped vortex that can be easily fabricated by ion-etching techniques and that needs no additional optics to work optimally. We will show coronagraphic performance from numerical simulations as well as laboratory validation in visible light. P5-09 Continuous phase mask We present numerical simulations and test laboratories of a phase mask coronagraph whose “à la four-quadrant” design was optimized by ajusting a law which is a ratio of polynomials in cos and sin so that the optimized for bandpass is increased and the chromatism well improved with respect to conventional four- achromatism and quadrant phase mask coronagraphs. The device was manufactured using ion-etching technique. bandpass. We show that the main limitation of performances comes from the most central region of the device where digitizing of levels of etching has a clear effect. Despite of that, the test on the Daniel Rouan bench showed that indeed there is a significant improvement in terms of spectral bandpass. (LESIA Observatoire de Paris) P5-10 Combination of Aiming at detecting and characterizing exo-planets, high-contrast coronagraphs have been apodized pupil and developed. We have tested mainly an eight-octant phase mask (8OPM), one of vortex phase phase mask mask family, manufactured by photonic-crystal space-variant wave plates at a focal plane of the coronagraph for coronagraph. A super-achromatic masks have been designed and fabricated both for near-IR Subaru Telescope ground-based observations and space observations in visible. To obtain a high-contrast with a non-circular aperture which has a secondary and spider shadows we applied a pupil apodizer (binary shaped pupil) in combination with the phase-mask coronagrarph. We have calculated Jun Nishikawa the pupil shape for WFIRST, SPICA, Subaru, and so on, achieving 1E-10 contrast with the (NAOJ/SOKENDAI/AB 8OPM or other masks. We have fabricated a shaped pupil for a Subaru-like aperture by chrome C) etching and obtained a high-contrast region of 1E-5 level at about 2 to 10 lambda/D without AO system in a lab. Next we have adjusted the target contrast to a suitable level (log contrast is -4.6 to -6.6) in the apodizer design for Subaru Telescope, because achievable contrasts by AO- corrected wavefronts at ground-based telescopes were often limited. Then we have obtained a large working angle of about 2 to 15 lambda/D and a 50% transmission, where we used a new pupil design of SCExAO. It will work at wide wavelength band of J, H, and K band without loss of the adjusted contrast. We are planning to test this apodizer with the achromatized 8OPM

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mask in the lab and install to the SCExAO at Subaru Telescope to achieve wide-band high- contrast observations at IR wavelength. P5-11 Polychromatic analysis The modular design of the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) of the coronagraphs in instrument allows laboratory and on-sky testing of innovative technologies necessary for future SCExAO ground-based and space high-contrast instruments. With a combination of optics wheels in various planes, it is possible to test a variety of high-performance coronagraphs dedicated for high-contrast at small inner working angle (1-3 lambda/D). SCExAO is now equipped with Julien Lozi several types of high-performance coronagraphs and apodizing optics, allowing for dozens of (NAOJ - Subaru combinations that are ready for science operations. Some are optimized for a specific band Telescope) (typically H-band), while others for broadband operation (J to K-band), used with the low- resolution mode of the integral field spectrograph CHARIS. The different options include: classical broadband Lyot coronagraphs with several occulter sizes, H-band vortex, H-band and broadband Phase-Induced Amplitude Apodization Complex Mask Coronagraphs (PIAACMC), Modified PIAA (MPIAA) optics that remove the central obscuration for phase mask coronagraphs (8-octant phase mask coronagraph (8OPM) or the vortex), a shaped pupil mask, as well as a vector Apodizing Phase Plate (vAPP) coronagraph. Here we present and compare the laboratory and on-sky performance of these coronagraphs. In particular we focus on the polychromatic contrast, throughput, inner-working angle and other parameters, as well as the impact of their performance for science operations. This study shows that some coronagraphs are more suited for median seeing or higher telescope vibrations, while others are ideal for good seeing. Some coronagraphs are also more adapted to speckle control algorithms like speckle nulling. The SCExAO experience shows that it is crucial for future ground-based high-contrast instruments to have some flexibility in coronagraphic performance to adapt to the observing conditions. P5-12 Chromatic High-contrast imaging instruments aim at directly imaging the exoplanets and characterizing Performance Of A their atmospheres by spectroscopy. Such instruments are usually equipped with coronagraphs Vector Vortex which attenuate the diffraction features of the star and enable the planet light detection. To Coronagraph obtain the spectra of exoplanets, coronagraphs must be efficient over large spectral bandwidth. One solution reaching bandpass larger than 30% is based on a “vector vortex” phase mask made of liquid crystal polymers. Such a mask theoretically creates an achromatic phase ramp and is Coline Lopez foreseen for several space or balloon missions. However, this mask has manufacturing defects (Paris Observatory, which deteriorate its chromatic performance. To filter these defects, it has been proposed to LESIA) place the vortex mask between two achromatic circular polarizers, which will not be perfect either. To characterize the performance of real vector vortex coronagraphs (VVC), we first develop an analytic formalism that takes into account the defects of the VVC and of the achromatic quarter wave plates used in the circular polarizers. We then perform the laboratory test of the VVC mask on the high-contrast imaging THD2 testbed at the Observatory of Paris. The preliminary laboratory results show an achromatic attenuation of the star by a factor 1e5 within 1 L/D between 600 to 800 nm in raw images. P5-13 SLM-based Digital In the last 3 years, we initiated a research effort to evaluate how liquid-crystal on silicon Adaptive (LCOS) spatial light modulator (SLM) panels would perform as programmable focal-plane Coronagraphy: Status, phase mask (FPM) coronagraphs, potentially allowing to replace static pre-manufactured performance update, components commonly used in high-contrast exoplanet imaging instruments with a versatile and future prospects alternative. We started to unveil how such an “adaptive coronagraph” could potentially help adapt to observing conditions and simultaneously serve the purpose of a wavefront sensing (WFS) device, hence making an optimal use of the scarce amount of available telescope time, Jonas G. Kuhn but also tackle specific science cases such as multiple-stars systems. In the near-future, such (Center for Space and dynamically-reconfigurable FPMs may also find high relevance in the context of non-ideal Habitability (CSH), segmented telescope pupils, or could be used for synchronous detection of faint incoherent University of Bern) astrophysical signals immerged in the coherent stellar noise. Here we present a status update on this work, notably the laboratory coronagraphic performance of two LCOS SLMs from different manufacturers, under broadband light conditions in the visible spectrum. We will also expose promising near-future technological developments that could turn the table around regarding astronomical usage scenarios, including faster and new polarization-insensitive LCOS panels, which we intend to test in the upcoming months. Finally, we unveil the PLACID instrument concept, the Programmable Liquid-crystal Adaptive Coronagraphic Imager for the DAG observatory, a 4-m Ritchey-Chrétien telescope built by Turkey in Eastern Anatolia. With a first light planned for late 2021, the DAG telescope will benefit from an extreme-adaptive optics system based on a pyramid WFS and a Alpao 468-DM, and equip a near-infrared HAWAII-

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2RG scientific focal-plane array. The near-infrared PLACID instrument is foreseen to be installed in-between these two sub-systems by mid-2022. P5-14 Towards High The next generation of large space-based observatory has the potential to detect and Throughput and Low- characterize dozens of Earth-like exoplanets. The largest possible exo-Earth yields can be Order Aberration obtained with proposed telescopes with central obstructions that allow for primary mirrors with Robustness for Vortex diameters greater than 10 meters. Unfortunately, use of most coronagraph designs on a Coronagraphs with telescope with a central obstruction entails significant losses in planet throughput, inner Central Obstructions working angle, or low-order aberration sensitivity in order to directly image exo-Earths. We address this limitation by examining a parameter space of coronagraph designs related to the apodized vector vortex coronagraph with the goal of simultaneously maximizing planet Kevin Fogarty throughput while minimizing inner working angle and sensitivity to low order aberrations. We (California Institute of discuss designs variations including pupil-plane apodizations that can be partially achieved with Technology) simple shaped-mirror prescriptions and use of multi-stage vortex coronagraphs. We present results based on the charge 6 vector vortex that have starlight suppression, and tip/tilt, astigmatism, and defocus sensitivities comparable to the charge 6 on a monolithic pupil. Compared to previous results for low-order aberration robust apodized vortex coronagraphs on on-axis designs, we report gains in throughput of a factor of >2 for every configuration examined, with an inner working angle similar to the charge 6 vortex. We also discuss potential application for the design space we consider to ground-based observatories with larger central obstructions but lower contrast requirements (e.g. 10-8 vs 10-10). Finally, we consider strategies for overcoming difficulties in aligning the elements of a multi-stage vortex coronagraph. P5-15 Heritage of technology This presentation reviews heritage of technology for mid-infrared coronagraph, which is for mid-infrared developed for space infrared telescopes for exoplanet science via spectroscopy and imaging. coronagraph onboard High-contrast observation in mid-infrared is complementary with visible wavelength region. space-borne telescopes Cryogenic unique technology is required for space-borne mid infrared coronagraph. for exoplanet Studies for binary shaped pupil mask coronagraphs are presented, which includes laboratory characterization demonstration of principle, design for on-axis telescopes, and development of free-standing pupil mask for mid-infrared. Another key technology is cryogenic active optics. 32 x 32 MEMS deformable mirror is developed and demonstrated in 4 K environment. Other kind of wavefront Keigo Enya correction mirrors, cryogenic tip-tilt mirror, and full-metal reflective optics (i.e, both mirrors (JAXA/ISAS) and other structures) are also developed. P5-16 Imaging short orbit After five years of operation, the current generation of ground-based exoplanet imagers such as exoplanets from the VLT/SPHERE and Gemini/GPI observe circumstellar environments by routinely achieving a ground with novel 105 contrast at 300 mas from an observed star. After surveying hundreds of stars, these Apodized Pupil Lyot instruments have enabled a handful of discoveries of gaseous planets at orbits wider than 5 AU, Coronagraphs possibly revealing their low occurrence at these separations. The existence of exoplanets at shorter distances is suggested by other detection methods. Observing these companions with the current facilities requires upgrades in all aspects (extreme adaptive optics, coronagraphy, and Mamadou N'Diaye post-processing methods) to achieve better contrast (>105) at shorter separations (<300mas). (Observatoire de la Cote In coronagraphy, many flavours have been developed over the past few years. The Apodized d'Azur) Pupil Lyot Coronagraph (APLC) is one of the leading types of coronagraphs in the current generation of exoplanet imagers, allowing a possible and easy implementation of new designs with improved inner working angle and contrast in these instruments. On SPHERE, the current APLCs use a prolate apodization, enabling a 105 raw contrast at 300mas on sky. We propose new APLC designs to observe planets with similar or better contrasts down to 150 mas. Based on shaped-pupil type optimization, these new designs rely on an optimal apodizer with a given throughput to maximize starlight rejection for a given area in the star image. We determine their raw contrast in the presence of AO residuals, instrumental aberrations, jitter, and other noise sources. Their detectivity levels are thus estimated after image post-processing on coronagraphic images and compared with the current designs to underline their gain in realistic conditions. We conclude on the relevance of these new designs to observe planets below 5AU with the current exoplanet imagers and discuss their potential for exoplanet observation with the ELTs. P5-17 Developing and Imaging rocky planets in reflected light, a key focus of future NASA missions and ELTs, Demonstrating Linear requires advanced wavefront control to maintain a deep, temporally correlated null of stellar Dark Field Control for halo at just several diffraction beam widths. We present the first laboratory tests of the Linear Exo-Earth Imaging Dark Field Control (LDFC) method at contrasts and separations required to image exo-Earths with the Ames around low-mass stars with future ground-based 30m class telescopes, using the Ames Coronagraph Coronagraph Experiment testbed. LDFC uses the response to perturbations in uncorrected, Experiment Testbed 'bright field' regions to maintain a dark hole without continuous DM probing. Our results show

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LDFC able to restore a dark hole whose contrast is degraded by up to a factor of 10 by perturbations and maintain this dark hole. We present preliminary results showing its efficacy Thayne Currie under a range of DM perturbations, describe current limitations/challenges, and discuss future (NASA-Ames Research plans for testing LDFC at raw contrasts needed to image solar system-like planets (including Center) Earths) around Sun-like stars. P5-18 Theoretical Obstructed and segmented apertures are common in exoplanet imaging telescopes and concepts. Performance Limits for In particular, the WFIRST, LUVOIR, and HabEx telescopes have obstructed or segmented Coronagraphs on apertures as a baseline or option. Most ground-based observatories have obstructed apertures, Obstructed and and many exoplanet imaging space telescope concepts based on an unobstructed aperture (e.g. Unobstructed Exo-C, ACESat) can benefit from having an obstructed one. A number of coronagraph designs Apertures: How Much have been developed for obstructed apertures, but usually suffer a substantial performance hit Can Current Designs compared to unobstructed aperture designs. Fortunately, the performance of obstructed be Improved? coronagraph designs seems to be steadily improving. We explore the extent to which the performance of coronagraphs on segmented apertures can be improved in theory, before fundamental physics limits are reached. Our methods involve Ruslan Belikov generalizing some of the treatment for coronagraph theoretical limits from Guyon et al. 2006 to (NASA Ames Research obstructed apertures, and extending it to higher order coronagraphs. We show that a Center) fundamental trade exists between the contrast, inner working angle, and sensitivity to stellar angular size. We also show that arbitrary tolerance to stellar angular size can be achieved at the cost of inner working angle. We present the effects of aperture obscuration and segmentation on these performance limits and trades, and show that although there is a performance degradation, it is not very strong. This implies that there is still a lot of room for performance improvement for current coronagraph designs on obstructed apertures. Although it is not known whether our performance limits can be reached with existing coronagraph architectures, they can at least be reached with a “brute- force” collection of ideal beamsplitters and masks. Our limits can thus be used as a target for future coronagraph technology development, as well as to show how much improvement in mission yields remains possible for any given aperture. P5-19 Sensitivity to telescope Future space missions such as the Large UV-Optical-Infrared Surveyor (LUVOIR) and the aberrations for Habitable Exoplanet Observatory (HabEx) require large apertures and coronagraphs with active exoplanet detection wavefront control to be able to suppress the starlight so faint planets can be detected and with the LUVOIR characterized adjacent to their parent star. coronagraph The Extreme Coronagraph for Living Planet Systems (ECLIPS) is the coronagraph instrument instrument ECLIPS on the LUVOIR Surveyor mission concept, an 8-15m segmented telescope. ECLIPS is split into three channels: UV (200 to 400 nm), optical (400 nm to 850 nm), and NIR (850 nm to 2.0 microns), with each channel equipped with two deformable mirrors for wavefront control, a Roser Juanola-Parramon suite of coronagraph masks, a low-order/out-of-band wavefront sensor, and separate science (NASA Goddard Space imagers and spectrographs. Flight Center) The Apodized Pupil Lyot Coronagraph (APLC) and the Vector Vortex Coronagraph (VVC) are the baselined mask technologies for ECLIPS to enable the required 1E10 contrast for observations in the habitable zones of nearby stars. Their performance depends on active wavefront sensing and control, as well as metrology subsystems to compensate for static aberrations induced by segment errors (piston and tip/tilt, among others), secondary mirror misalignment, and global low-order wavefront errors. Here we present the latest results of the simulation of these effects for the two technologies, as well as the effects of dynamic aberrations such as segment jitter, segment drift and line of sight pointing errors, and discuss the achieved contrast for exoplanet detection and characterization. Finally, we show simulated observations using high-fidelity spatial and spectral input models of complete planetary systems generated with the Haystacks code framework, setting boundaries for tolerance of such errors. P5-20 SISTER: Simulating SISTER is a versatile, open source software written in Matlab that allows any astronomer to Exoplanetary Systems generate accurate images of exoplanetary systems as observed with a telescope and a starshade. as observed with The images can then be analyzed to determine which exo-planets are detectable and which Starshade atmospheres may be characterized in future instruments. SISTER has already been used in the mission design of a few NASA missions, including WFIRST, HabEx, and other mission Sergi Hildebrandt concepts. SISTER has a detailed on-line documentation including a tutorial with many (JPL/Caltech) examples.

P5-21 On-sky validation of Gas giant planets, brown dwarfs, and debris disks around nearby stars are now routinely the ZELDA wavefront observed by dedicated high-contrast imaging instruments on large, ground-based telescopes. sensor for the These facilities combine extreme adaptive optics and coronagraphy to achieve unprecedented

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calibration of non- sensitivities for exoplanet detection and spectral characterization. However, residual quasi-static common path phase aberrations in these systems represent a critical limitation for the detection of giant aberrations in planets with a contrast lower than a few 10-6 at separations smaller than 0.3”. A major source of VLT/SPHERE residual phase errors are the non-common path aberrations (NCPA) between the visible wavefront sensing path of the ExAO system and the near-infrared science path in which the coronagraph is located. In 2013 we proposed ZELDA, a Zernike wavefront sensor to measure Arthur Vigan NCPA at nanometric accuracy in coronagraphic instruments. A prototype was installed in (Laboratoire VLT/SPHERE in 2014 and we previously demonstrated our ability to measure and compensate d'Astrophysique de for the instrument's NCPA. In the present work, we move to the next step with the on-sky Marseille / CNRS) validation of the NCPA compensation with ZELDA. We demonstrate that the compensation works perfectly on-sky in closed loop, leading to an attenuation of the amount of aberrations by a factor ~2 and a measurable gain in raw contrast. We use coronagraphic image reconstruction based on a detailed model of the instrument to show that both internal and on-sky raw contrasts can be precisely explained. We establish that the observed performance of SPHERE after NCPA compensation is no longer limited by an improper compensation of the aberrations but by the design of the apodized-pupil Lyot coronagraph. We conclude with prospects for an upgrade of the SPHERE baseline coronagraph which would fully benefit from an improved NCPA compensation and for future exoplanet imaging facilities on the ground and in space (e.g. ELT, LUVOIR, HabEx). P5-22 Focal-plane wavefront High-contrast imaging instruments are currently limited by slowly evolving aberrations that are sensing with the vAPP: non-common and chromatic with respect to the main wavefront sensor arm and are therefore not on-sky demonstration detected. Focal-plane wavefront sensing (FPWFS) is a strongly preferred solution as it measures at SCExAO these quasi-static aberrations at the place where it matters: the science detector. Phase diversity methods have been successfully deployed on several testbeds and instruments, but in general suffer from a science duty cycle < 100% as several (defocused) images have to be taken. Here Steven Peter Bos we present a method where FPWFS is directly integrated in the vector Apodizing Phase Plate (Leiden Observatory) (vAPP). The vAPP is a pupil-plane coronagraph that manipulates phase to generate dark holes. The phase is induced through the inherently achromatic geometrical phase on the circular polarization states by a half-wave liquid crystal layer with a varying fast axis orientation. The coronagraph yields two point-spread functions (PSFs) with opposite circular polarization and opposite dark holes. The wavefront sensing capabilities are achieved by integrating the Asymmetric Pupil Fourier Wavefront Sensor in the vAPP. The asymmetric pupil shapes the coronagraphic PSFs such that they contain sufficient diversity to enable a one-shot phase estimation. This eliminates additional FPWFS holograms or DM probes and yields a 100% science duty cycle. We have developed a non-linear algorithm that performs a maximum- likelihood estimation of the phase by minimizing an objective function. We show, by idealised simulations, that for a sufficient photon number a nanometric accuracy can be reached. Using the vAPP installed within the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system we first demonstrate the feasibility of the algorithm with the internal source. Then, we present the on-sky performance of the algorithm by measuring and controlling the 30 lowest Zernike modes. P5-23 Overview of focal plane The Low Wind Effect (LWE) refers to a phenomenon that occurs when the wind speed inside a wavefront sensors to telescope dome drops below 3m.s-1. The LWE was identified as being induced by air correct for the Low temperature inhomogeneities across the pupil created by the temperature gradient near the Wind Effect on telescope spider. Those inhomogeneities produce phase discontinuities in the pupil plane that SUBARU/SCExAO cannot be detected and corrected by traditional Adaptive Optics (AO) systems such as the pyramid wavefront sensor or the Shack-Hartmann. Considering the pupil as divided in 4 quadrants by a regular spider, the phase discontinuities correspond to piston, tip and tilt Sebastien B. Vievard aberrations in each quadrant of the pupil. Uncorrected, it strongly decreases the ability of high (ABC, LESIA, Subaru contrast imaging instruments utilizing coronagraphy to detect exoplanets at small angular Telescope) separations. The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument at Subaru Telescope is affected by the LWE around 10 to 20% of the observing time. Its unique modular design makes it easy for any collaborator to test new concepts and algorithms. In the context of the LWE correction, multiple wavefront sensors are currently being developed and tested on SCExAO. Among them, the Zernike Asymmetric Pupil (ZAP) wavefront sensor already showed on-sky that it could measure the LWE induced aberrations in focal plane images by adding an asymmetric mask in the pupil plane. Other focal plane wavefront sensors that do not require extra-hardware are also investigated: A Point Spread Function reconstruction from the pyramid

52 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

wavefront sensor telemetry using neural network and different phase diversity algorithms using one or multiple images. We present the different algorithms and compare their implementation and efficiency on SCExAO/SUBARU as real-time wavefront sensors for the LWE compensation. This work should be useful in the context of extremely large telescopes where the dome might be subject to large air movements and temperature inhomogeneities. P5-24 Mach-Zehnder Extreme adaptive optics (XAO) has severe difficulties meeting the high speed (>1kHz), high Wavefront sensor for accuracy and photon efficiency requirements. The use of the self-referenced Mach-Zehnder XAO: From laboratory wavefront sensor allows counteracting these limitations in order to deliver the required high tests to on sky Strehl ratio for high contrast applications with ELTs. We will first describe the advantages and measurements using challenges of this scheme and present laboratory results obtained with an integrated version of the SCAO capability of the Mach-Zehnder WFS that opened the way to on-sky measurements. We will then present the CANARY at the results obtained with this WFS on sky at the William Hershel 4.2m Telescope using the SCAO William Hershel capability of CANARY. Telescope

Maud Langlois (CNRS/CRAL) P5-25 Deep Neural Networks In high-contrast imaging applications, such as the direct imaging of exoplanets, a coronagraph Improve the Dynamic is used to attenuate the light from an on-axis bright target such that a dimmer, off-axis object Range of Lyot-based can be imaged. To maintain contrast, the light entering the coronagraph must be aligned on-axis Low Order Wavefront with the coronagraph optics and other low-order aberrations must be minimized. Sensing Lyot Low-Order Wave Front Sensors (LLOWFS) use light rejected from the coronagraph's Lyot stop to make measurements of Tip, Tilt, Defocus, and higher-order terms. The LLOWFS are being increasingly used with phase mask coronagraphs, and have the advantage that they do Gregory W. Allan not degrade the system’s signal-to-noise ratio and do not exhibit non-common-path error. (Massachusetts Institute Unfortunately, conventional use of the LLOWFS is limited by its comparatively small linear of Technology) range of just tens of nm RMS wavefront error. In a closed-loop system, LLOWFS can be used out to their monotonic range of roughly 100 nm RMS. In-space and balloon-borne high-contrast imaging telescopes therefore include additional wavefront sensors to correct initial alignment errors of 100s of nm. Extending the useful range of the LLOWFS could allow these coarse wavefront sensors to be eliminated, reducing system complexity. To increase the dynamic range of the LLOWFS, we demonstrate the use of a deep neural network (DNN) to learn the nonlinear relationship between the LLOWFS sensor output and the wavefront shape in the pupil plane. We present a DNN design based on the residual network (ResNet) architecture. The proposed DNN can recover Zernike coefficients of linear combinations of 15 Zernike terms with amplitudes of up to 300 nm RMS. The recovered coefficient values are accurate to 20 nm RMS, which is well within the linear range of the sensor. This technique could thus be combined with conventional linear regression to enable the LLOWFS to perform all necessary low-order sensing. P5-26 Laboratory On cryogenic space-borne infrared telescopes, a figure error of the mirror surface due to a demonstration of a manufacturing error and/or thermal deformation can cause a wavefront error, which generates cryogenic deformable scattered light called speckles and makes the imaging performance worse. Particularly in direct mirror for wavefront observations of exoplanets by using a coronagraph, speckles become serious problem because correction of space- they degrade contrast of the point spread function (PSF) of the central star and drown out the borne infrared planet signals. telescopes For on-orbit wavefront correction, we developed a MEMS-processed electro-static deformable mirror (DM) with 1020 actuators and a special surrounding structure appropriate for use under the cryogenic temperature. We performed a laboratory demonstration of its operation in three Aoi Takahashi cooling cycles between 5 K and 295 K. Using a laser interferometer, we detected the (Astrobiology Center deformation corresponding to the applied voltages under the cryogenic temperature for the first (ABC)) time. The relationship between voltages and displacements was expressed by a quadratic function, which is qualitatively expected from the principle of electro-static DMs. We also found that it had a high operating repeatability of a few nm root-mean-square and no significant hysteresis. Based on the measured values of repeatability, we simulated the improvement of a PSF contrast by the wavefront correction with our DM. Assuming an example of shaped pupil mask coronagraph, the PSF contrast was found to be improved up to 10-7 – 10-6 in the dark region, although its contrast is 10-6 – 10-4 without DM.

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Such cryogenic DM with multi actuators has a worldwide uniqueness. If it is realized to be mounted on space-borne infrared telescopes, it will be so useful not only for application to the direct observation of exoplanets, but also for lower-cost and shorter-term development of space- borne telescopes in terms of relaxing requirements to a figure error of the mirror surface. P5-27 Results with FALCO, a FALCO, an open-source software package for coronagraphic wavefront correction, enables the Software Package for high-contrast imaging community to easily learn and build upon previous work. After the Coronagraphic development of open-source libraries for optical propagation (e.g., PROPER and POPPY), there Wavefront Correction was a need for a common, validated software platform for sharing established algorithms and testing new ones. Meeting this need, FALCO provides an expandable framework containing working examples of pair-wise probing estimation and electric field conjugation (EFC) control. A J Eldorado Riggs Several papers have been written using FALCO to demonstrate new coronagraph designs or (Jet Propulsion wavefront sensing and control algorithms. At both Caltech and JPL, FALCO is being used to Laboratory) run high-contrast testbeds. JPL and NASA GSFC use FALCO for end-to-end coronagraph instrument modeling for the WFIRST mission and the LUVOIR mission concept. Here we describe FALCO's capabilities and its various results in coronagraph design, modeling, and testbed operation. P5-28 Wavefront control and The Wide Field Infrared Survey Telescope's Coronagraph Instrument (WFIRST CGI) is a high- calibration for the contrast imaging system which will fly as a technology demonstration instrument for exoplanet WFIRST Coronagraph imaging at a final contrast goal of ~1e-9. To achieve this depth of starlight suppression, CGI Instrument will have control loops for both low- and high-order wavefront control. Low-order loops will correct for fast line-of-sight jitter and slower thermally-induced wavefront aberrations based on measurements from a Zernike wavefront sensor, while high-order wavefront control will null Eric Cady out quasistatic speckles with a final contrast goal of ~1e-9. We give an overview of our (Jet Propulsion wavefront control architecture and baseline algorithm choices, as well as some of the associated Laboratory, California challenges, including self-calibration, model validation and performance verification, and Institute of Technology) operation within the limited capabilities of flight-qualified hardware. P5-29 Applications of Multi- To enable the detection and characterization of exoplanets in planetary systems near to our own, Star Wavefront high-contrast imaging techniques must be developed and their expected performance verified. Control to WFIRST, High-contrast imaging capabilities with both coronagraphic and starshade architectures are HABEX, and LUVOIR planned for NASA's suite of upcoming space missions including the Wide Field Infrared Survey Telescope (WFIRST) and its Coronagraphic Instrument (CGI) demonstrator and two missions concepts currently being reviewed by the Decadal Survey: the HABitable Worlds EXplorer Dan Sirbu (HABEX) and the segmented Large UV/Optical/IR (LUVOIR). All these missions will feature (NASA Ames Research suppression of on-axis starlight caused by both diffraction and aberration-induced leakage. Center / BAERI) The majority of nearby FGK stars are located in multi-star systems which exhibit additional leakage from the off-axis companion star that may be brighter than the target exoplanet. Multi- Star Wavefront Control (MSWC) is a wavefront-control technique that allows simultaneous suppression of starlight of both stars in a binary system using the existing wavefront control system on planned coronagraphic instruments. MSWC would thus enable direct imaging of circumstellar planets in binary star systems increasing the pool of target stars available. These binary stars would include high-quality nearby targets such as both Alpha Centauri stars for which a rocky planet in reflected light would be more easily detectable and characterizable than other targets. Here, we briefly discuss the principles of MSWC and present the latest milestone results of our technology development program featuring applications of MSWC to the suite of future space telescope missions. We demonstrate simulated high contrast imaging capabilities of multi-star systems for several instruments including: (1) WFIRST with the Shaped Pupil Coronagraph (SPC) and the proposed Starshade Probe, (2) monolithic HABEX pupil using the Vector Vortex Coronagraph (VVC), (3) segmented LUVOIR-B pupil using the VVC, and (4) a small aperture Alpha Centauri direct-imager mission concept using both the VVC and PIAA coronagraph. We compare the single-star performance for each case before demonstrating the multi-star imaging mode. P5-30 Wavefront Control and Achieving high contrast on segmented, obscured apertures requires the combination of Modeling for High optimized coronagraphs with wavefront control strategies for phase and amplitude, including Contrast on Segmented control loops operating on multiple timescales. We present results using Optimized Stroke Apertures: Results Minimization and APLC coronagraphy on the HiCAT testbed to achieve deep contrast on a from the HiCAT segmented pupil, and discuss several factors affecting performance. High-fidelity end-to-end Testbed numerical modeling is a key enabling tool for optimizations, operation of model-based control, and analysis of performance. As part of our technology demonstration program we have developed a high-fidelity numerical model of the HiCAT testbed, tightly coupled to calibrated Marshall Perrin hardware parameters. Using this numerical model we present current understanding of the

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(STScI) achieved contrast error budget on HiCAT, and models for system performance as we progress towards demonstrations of high contrast on dynamic time-variable segmented apertures. P5-31 Comparing Focal Plane Next generation of space-based instruments such as WFIRST, LUVOIR or HabEx aims to Wavefront Sensors on observe circumstellar environments to detect objects 1010 times fainter than their stars. THD2 bench : Self- However, direct imaging at this level of contrast requires a wavefront sensor in the focal plane coherent camera, Pair to control quasi-static aberrations which slowly change in time with thermal and mechanical Wise Probing and instabilities in the instrument. The wavefront sensor has to be fast enough and reach a COFFEE subnanometer accuracy in the estimation of both amplitude and phase aberrations, with minor changes in the instrument optical path. In this presentation, we compare three focal plane wavefront sensors that estimate the electric Axel Potier field of the stellar speckles from the science image: (LESIA - Observatoire 1) the Self-Coherent Camera which spatially modulates the speckle intensity in the final image, de Paris) 2) pair wise probing and 3) the coronagraphic phase diversity COFFEE, which temporally modulate the speckle intensity using phase diversities. Our study compares their abilities to estimate a given wavefront aberration using numerical simulations and laboratory tests on the THD2 testbed. Then, they are associated with the same wavefront control technique to study the capacity to dig a dark hole in the image with contrast level below 10-⁸ with one deformable mirror both from numerical simulations and in the laboratory. Eventually, we show the advantages and drawbacks in the use of these different wavefront sensors. P5-32 Overview of the THD2 Characterization of exoplanet atmospheres at long period requires direct imaging and performance spectroscopy of the planetary system. Actual instrument like SPHERE/VLT, GPI/Gemini, SCExAO/Subaru are already able to study a handful of young giant planets. Soon, the coronagraphic capability aboard the JWST should allow an improvement of our spectral Pierre Baudoz knowledge of these planets but the spectroscopic study of mature giant planets and lower mass (Observatoire de Paris) planets (Neptunes, Super Earths) requires the achievement of better coronagraphic performance. Space-based coronagraph on WFIRT-AFTA should start to improve this study at low spectroscopic resolution but dedicated projects on large space telescope and on the ELT will be required for a complete spectroscopic analysis of Neptune and Super Earth planets. The performance of actual instrument is still 3 to 5 order of magnitude away from the one required for such analysis. To prepare these new instruments, we developed a high contrast imaging bench called THD2, which can each contrast level better than 108. This optical bench can simulate either the beam provided by a space telescope or the first stage of adaptive optics behind a ground-based telescope. Through worldwide collaborations in the last 5 years, the bench has been used to test more than 8 different coronagraphs, to compare 3 focal plane wavefront sensor techniques and to study Dark Hole optimization using two deformable mirrors. After describing the THD2 bench, we will give an overview of the recent results obtained on achromatic coronagraphs, on amplitude and phase correction using 2 DM, and on the comparison of several focal plane wavefront sensors either for space-based environment or for a second stage correction behind adaptive optics. P5-33 The Parabolic One of the primary goals of future coronagraph space missions is to spectrally characterize Deformable Mirror Earth-like exoplanets. The spectrum in multiple bands must be taken to constrain their Testbed at Goddard molecular abundances, requiring multiple measurements be take to achieve the final science. Space Flight Center Individually, these measurements are challenging since we must achieve high contrast and the dispersed signal requires much longer exposure times. Observing efficiency is critical and directly related to how large of a field of view we can correct and the bandwidth of that Tyler Groff correction. In addition to the coronagraph itself, the bandwidth and depth of contrast is related (NASA GSFC) to the wavefront control system, which classically uses two deformable mirrors (DMs) in series. The minimum distance between these DMs is determined by the Talbot distance of the beam, meaning it scales as the square of the beam size. We are exploring an alternative design architecture to the two-DM approach in which the reimaging optics for the coronagraph are also deformable and we only retain a high order pupil DM. With these off-axis parabolic elements being made deformable, the long propagation distance between the two DMs is eliminated. Additionally, by using multiple surfaces we find in simulation that we may reduce the actuator count on individual parabolic surfaces. Controlling the aberrated surfaces directly, we investigate whether we can improve controllable bandwidth and achieve a more robust wavefront solution. To test our models and demonstrate achievable performance, Goddard is working with vendors to provide custom fabricated off-axis parabolic DMs and building a testbed using these DMs. Here we show the testbed and parabolic deformable mirror

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development effort, simulated results, and the experimental results to date of the base experiment which include low order wavefront sensing methods. P5-34 Assembly, Integration, The Deformable Mirror Demonstration Mission (DeMi) is a 6U CubeSat that will operate and and Testing of the characterize the on-orbit performance of a Microelectromechanical Systems (MEMS) Deformable Mirror deformable mirror (DM) with both an image plane wavefront sensor and a Shack-Hartmann Demonstration Mission wavefront sensor (SHWFS). Coronagraphs on future space telescopes will require precise (DeMi) CubeSat wavefront control to detect and characterize Earth-like exoplanets. High-actuator count MEMS Payload DMs can provide wavefront control with low size, weight, and power. The DeMi payload will characterize the on-orbit performance of a 140 actuator MEMS DM with 5.5 μm maximum stroke, with a goal of measuring individual actuator displacement contributions to 12 nm and Rachel Elizabeth Morgan correcting static and dynamic phase errors to less than 100 nm RMS. The 140 actuator MEMS (MIT Department of DM DeMi is demonstrating in space is manufactured using the same techniques as the higher Aeronautics and actuator count MEMS DMs proposed for future space telescopes. The payload contains Astronautics) miniaturized DM drive electronics to fit within the CubeSat form factor and uses two cross- strapped Raspberry Pi 3s as flight computers to control the DM and wavefront sensor cameras. We present an overview of the payload design, the assembly, integration and test process, and report on optomechanical calibration and performance results pre- and post-integration with the bus. The DeMi payload is ~4.5 U in volume 2.5 kg in mass, and is flying on a 6 U spacecraft built by Blue Canyon Technologies. Launch is planned for late 2019. P5-35 New high contrast The High-Contrast Spectroscopy Testbed for Segmented Telescopes (HCST) in the Exoplanet technology Technology Laboratory (ET Lab) at Caltech is designed to fill the technology gap that will demonstrations at the enable direct imaging and characterization of exoplanets with future segmented ground-based, High-Contrast and space-based telescopes. Wavefront sensing and control experiments at HCST using the Spectroscopy Testbed algorithm known as electric field conjugation (EFC) have achieved a raw contrast of 1x10-8 on for Segmented one-sided dark holes for monochromatic light at 775 nm, and 3x10-8 for 10% broadband light at Telescopes (HCST) 775 nm, both for a clear aperture telescope configuration. Here we present the current status on the experiments with an apodized vortex coronagraph (AVC) using a LUVOIR-B type segmented aperture. Preliminary results yield a raw contrast of 1x10-8 on one-sided dark holes Jorge Llop Sayson for monochromatic light at 775 nm. We also present the status of the fiber injection unit, in (California Institute of which we aim to reach levels of 10-9 raw contrast in broadband light through a single mode Technology (Caltech)) fiber, and to demonstrate multi-object wavefront control with multiple fibers.

P5-36 Performance SPHERE has discovered a multitude of circumstellar disks, two new directly imaged planets, simulations of the high- and has provided constraints on planet occurrence around young stars. Unfortunately, with its res characterization of low resolution spectrographs, it has limited capabilities to thoroughly characterize the planetary directly imaged planets atmospheres. High resolution spectroscopy (R = 100K) has proven to be a crucial tool that with HiRISE provides detailed knowledge on atmospheric composition, rotation and orbital motion, but is currently not available in combination with the high contrast capabilities provided by Extreme AO and coronagraphs. Gilles Otten HiRISE, a proposed coupling between SPHERE and CRIRES+ at VLT/UT3 will enable high- (Laboratoire resolution spectroscopy of directly imaged exoplanets in the regime of Extreme AO. This d'Astrophysique de allows the improved study of formation processes and detailed composition in young giant Marseille) exoplanets. Here I will present simulations of HiRISE's performance that are based on realistic estimates of throughput and noise from SPHERE, CRIRES+ and HiRISE. From spectra of planet and host star we calculate the SNR for the detection of atmospheric species in the atmospheres of these exoplanets, as well as the accuracy on their velocity dispersion and radial velocities. The influence of coronagraph choice and grating setting is evaluated and the performance of HiRISE is compared to that of CRIRES+ by itself, and also, in combination with a dedicated local spectrograph. Lastly, we show for a grid of planet separation and planet-star contrast the improvement that HiRISE can give for future planet detections (e.g., Gaia astrometric planets). In a baseline instrument design that can be implemented on a short timescale, HiRISE is shown to outperform CRIRES+ for planets close to the star, with up to a factor of 10 improvement in observing efficiency. P5-37 The Promise of Advances in Adaptive Optics have made it possible to develop a new generation of very high Diffraction Limited spectral resolution spectrometers R~(100,000-180,000) operating in the deep red and near-IR on Spectrometers for large telescopes. These instruments can be used for direct spectroscopy of exoplanets, precision Exoplanet radial velocity (PRV) measurements when coupled to a high precision calibration source, as Characterization well as for a variety of general astrophysics programs.

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Feeding a diffraction-limited beam into a single mode fiber has many advantages: the small Charles Beichman A*Omega of a diffraction-limited beam enables a much more compact instrument than a (NASA Exoplanet seeing-limited one; a compact instrument is easier to maintain under precise thermal control for Science Institute/IPAC) high opto-mechanical stability; the use of single mode fibers eliminates mode scrambling and many PRV error budget terms related to instrument point spread function and telescope pointing; and finally a compact instrument is inherently lower cost than a much larger seeing- limited one. We are presently commissioning the Palomar Advanced Radial Velocity Instrument (PARVI) for the Palomar 5-m telescope, and designing more ambitious diffraction limited spectrometers: HISPEC for Keck, and MODHIS , a potential first light instrument for TMT. We will discuss early commissioning results from PARVI and plans for HISPEC and MODHIS. Finally, we note it will be possible to extend these benefits into visible wavelengths as AO advances to shorter wavelengths and ultimately to a space-based telescope such as the EarthFinder. P5-38 Progress Towards a Single-mode fibers are a promising technology for improving the efficiency of exoplanet Laboratory characterization observations with a coronagraph. Recent simulation results have shown that Demonstration of a they offer the potential for improved spectral bandwidth, higher usable throughputs, and Multi-Object, Single- improved rejection of exozodi when used as an integral part of the starlight Mode Fiber suppression/wavefront control system of a coronagraphic instrument. We report here on Spectrograph progress towards a laboratory demonstration of this capability. Using a multicore single-mode fiber, we will be able to explore the multi-object capabilities of this configuration, as well as test the limits of achievable spectral bandwidth and achievable contrast. We present our Carl Coker experimental setup as well as simulations of expected system performance on the High Contrast (Jet Propulsion Testbed for Segmented Telescopes (HCST) at Caltech. Laboratory) P5-39 Spectroscopy below the FIRST (Fibered Imager foR a Single Telescope instrument) is a post-AO instrument that diffraction limit with enables high contrast imaging and spectroscopy at spatial scale below the diffraction limit. FIRSTv2 at the Subaru FIRST achieves sensitivity and accuracy by a unique combination of sparse aperture masking, Telescope spatial filtering by single-mode fibers and cross-dispersion in the visible. The telescope pupil is divided into sub-pupils by an array of microlenses, coupling the light into single-mode fibers. The output of the fibers are re-arranged in a non redundant configuration, allowing the Elsa Huby measurement of the complex visibility for every baseline over the 600-900nm spectral range. (LESIA, Observatoire de In this presentation, we will report on the on-sky results obtained with FIRST in its current Paris) design, as a module of the SCExAO extreme adaptive optics instrument on the 8-m Subaru telescope. On-sky commissioning data show the detection of several stellar companions, and in particular of the Alpha Equu binary system angularly separated by 0.6 λ/D (11mas). Even at such a separation, FIRST delivers information on the companion spectrum, providing valuable constraints on the stellar parameters of the system such as the effective temperatures and surface gravity. The second part of this presentation will focus on the ongoing instrument upgrades, which aim at increasing the instrument’s stability and sensitivity, thus improving the dynamic range. We initiated a comprehensive upgrade of FIRST’s interferometric scheme, based on a new series of photonic on-chip beam combiners. The new chip includes waveguides in crystalline electro-optic material (Lithium Niobate) that will enable on-chip active phase control of the light at high speeds (up to MHz) for the first time in an astronomical interferometric instrument. Coupling high angular resolution and spectral resolution in the visible, FIRST offers unique capabilities in the context of the spectral characterization of close companions. As a conclusion, we extrapolate a similar approach on a 30m-class telescope, which would provide unique scientific opportunities for companion detection and characterization at very high angular resolution. P5-40 An Introduction to The Santa Cruz Array of Lenslets for Exoplanet Spectroscopy (SCALES) is a proposed 2-5 SCALES, the Next- micron, diffraction-limited integral field spectrograph for the WM Keck Observatory currently Generation Exoplanet in advanced conceptual design, and is functionally the ‘red arm’ of the Planetary Systems Spectrograph Instrument (PSI) for the Thirty Meter Telescope (TMT). Its fully cryogenic optical train uses a custom silicon lenslet array, selectable coronographs, and dispersive prisms to carry out integral field spectroscopy over a 3.6 arcsec field of view with low spectral resolution (R~50 to 200). A Richard Deno Stelter set of insertable mirrors relay light to and from a slicer module sitting behind the lenslet array (UCO/UC Santa Cruz) allows for medium spectral resolution (R~5000 to 10,000), which until SCALES has not been available at the diffraction limit behind a coronagraph at these wavelengths. The opto- mechanical design takes advantage of modern diamond-turning materials and machining techniques with minimal risk and cost while delivering diffraction-limited performance both at Keck and TMT. Unlike previous IFS-based exoplanet instruments, SCALES is capable of

57 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

characterizing cold exoplanet and brown dwarf atmospheres (<600 K) at bandpasses where these bodies emit most of their radiation while capturing interesting molecular spectral features. We have also developed tie-ins for focal-plane wavefront sensing and high-dispersion coronagraphic spectroscopy (R~100,000) using fully cryogenic fiber injection and extraction units and spectrographs based on at CalTech. I will introduce the opto-mechanical design and discuss the exoplanet science driving the design of SCALES/PSI-Red. P5-41 Partially Filled The exponential growth in exoplanet studies and science cases such as detecting life and even Aperture civilizations on Earth-like planets requiring high contrast observations is a powerful reason for Interferometric developing very large optical systems optimized for narrow-field science. New concepts, which Telescopes Achieving cross the boundary between fixed aperture telescopes and interferometers, combined with Large Aperture and technologies that decrease the system moving mass, can violate the cost and mass scaling laws Coronagraphic that make conventional large-aperture telescopes relatively expensive. Here we describe a new Performance — The concept and a new technology for creating extremely lightweight diffraction-limited meta- Exo-Life Finder (ELF) material-based optical surfaces systems, which breaks this scaling relation in a large optical/IR Telescope. system dedicated to high dynamic science cases. Keywords: coronagraphic performance, hybrid very large telescopes, optical-hybrid-materials miror, redundant-baseline interferometry, phased array telescope, high-dynamic range GIL MORETTO observations (Centre de Recherche Astrophysique de Lyon- CRAL/CNRS, Saint- Genis Laval, 69561, FRANCE) P5-42 Vortex Fiber Nulling Vortex fiber nulling (VFN) is a new interferometric method for suppressing starlight in order to for Exoplanet observe exoplanets at small angular separations from their star, 1λ/D. This technique may Observations: Concept, enable the discovery of young giant planets at separations smaller than conventional Laboratory Results, coronagraphs can achieve, as well as the spectral characterization≲ of RV-detected exoplanets and Planned On-Sky that are currently unreachable by conventional coronagraph systems. VFN relies on a vortex Deployment mask which prevents starlight from coupling into a single mode fiber while still coupling up to 20% of the planet light into the fiber which can then be routed to a spectrograph for analysis. Monochromatic starlight coupling fractions of 6x10-5 have already been demonstrated in the Daniel Echeverri lab with off-the-shelf optics and recent results have expanded the concept to broadband, (Caltech) polychromatic light. A VFN module will also be added to the new Keck Planet Imager and Characterizer (KPIC) instrument on the Keck II Telescope at Maunakea as part of the Phase II upgrade in 2020. This will provide extreme-AO observations of close-in exoplanets in K-band (2.2µm) with high-resolution spectra from the extant NIRSPEC spectrograph. Here we present the VFN concept, theoretical performance, design considerations, and latest laboratory results. We will also present the VFN module of KPIC including the instrument design, beam-shaping optics, and predicted on-sky performance based on the current AO performance from KPIC Phase I commissioning. P5-43 Detecting companions The Palomar Fiber Nuller (PFN) is a near-infrared nulling interferometer that achieves high inside the accuracies using a symmetric layout, single-mode-fiber beam combination, extreme adaptive coronagraphic regime optics pathlength and fiber-coupling stabilization, rapid signal detection and calibration, and a with nulling statistical null-depth fluctuation analysis that greatly relaxes the phase stabilization requirement. interferometry The PFN has enabled the demonstration of companion detection by means of nulling-baseline rotation, as originally envisioned for space-based nulling interferometry. It has also demonstrated techniques allowing improved interferometric accuracies (several 10e-4). In Eugene Serabyn particular, the spectroscopic binary eta Peg shows an approximately sinusoidal Ks-band null- (Jet Propulsion depth rotation curve due to a secondary star 1.08 ± 0.06 x 10e-2 as bright as the primary, at a Laboratory, California separation (30 mas) well inside both the telescope’s diffraction-limited beam diameter (87 mas) Institute of Technology) and typical coronagraphic inner working angles. A null-depth floor of 4.8 ± 1.6 x 10e-4 due to the primary star’s diameter was also detected. Potential nulling performance improvements as well as the use of larger telescopes can together enable a variety of small-angle observations inside the coronagraphic regime. P5-44 Robust high contrast The formation of inteferometric observables insensitive to first order phase perturbations such imaging with kernel- as closure- and kernel-phase used for low to moderate contrast detections relies on the linearity nulling interferometry properties of phase induced perturbations on the raw (Fourier-phase) observables. A high- contrast device such as a coronagraph or a nuller destroys this simple dependance and turns the original linear problem into a degenerate, highly-covariated one, dominated by second order Frantz Martinache

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(Universite Cote d'Azur, phase induced errors. The formulation of the general problem of kernel-coronagraphy is not Observatoire de la Cote straightforward. d'Azur, CNRS, A solution is however emerging in the case of a sparse four sub-aperture array feeding a Laboratoire Lagrange, modified four-beam nuller device, compatible with spectroscopy and designed to enable the France) formation of kernel-nulled outputs. These new high-contrast observables appear to be robust against second order perturbations and feature properties reminiscent of the kernel-phase. Envisionned application for this novel architecture include both sparse aperture masking and long baseline interferometry, therefore able to probe the high-contrast features of exoplanetary systems over a wide range of spatial scales. We will present the properties and features of the concept of kernel-nuller and those of its first near-infrared integrated optics prototype tested at Observatoire de la Côte d'Azur, in the context of the KERNEL project. P5-45 Implementing Multi- PHASECam is the fringe tracker for the Large Binocular Telescope Interferometer (LBTI). It is wavelength Fringe a near-infrared camera which is used to measure tip/tilt and fringe phase variations between the Tracking for the two AO-corrected apertures of the Large Binocular Telescope (LBT). Tip/tilt and phase sensing LBTI's Phase Sensor, are currently performed in the H (1.65 microns) and K (2.2 microns) bands at 1 kHz, and the K PHASECam band phase telemetry is used to send tip/tilt and Optical Path Difference (OPD) corrections to the system in order to maintain fringe coherence and visibility. However, due to the cyclic nature of the fringe phase, only the phase modulo 360 degrees can be measured. PHASECam's Erin Maier phase unwrapping algorithm, which attempts to mitigate this issue, occasionally fails in the case (University of Arizona) of fast, large phase variations. This can cause a fringe jump, in which case the OPD correction will be incorrect by a wavelength. This can currently be manually corrected by the observer. However, as the LBTI commissions further modes which require robust, active phase control and for which fringe jumps are harder to detect, including multi-axial (Fizeau) interferometry and dual-aperture non-redundant aperture masking interferometry, a more reliable and automated solution is desired. We present a multi-wavelength method of fringe jump capture and correction which involves direct comparison between the K band and H band phase telemetry. We demonstrate the method on archival PHASECam telemetry as well as telemetry from recent on-sky observations, showing it can provide a robust, reliable way of correcting fringe jumps in future LBTI observations. P5-46 Pushing the Limits of Further advances in exoplanet detection and characterisation require sampling a diverse Exoplanet Discovery population of extrasolar planets. One technique to detect these distant worlds is through the via Direct Imaging with direct detection of their thermal emission. The so-called direct imaging technique, is suitable for Deep Learning observing young planets far from their star. These are very low signal-to-noise-ratio (SNR) measurements and limited ground truth hinders the use of supervised learning approaches. In this paper, we combine deep generative and discriminative models to bypass the issues arising Kai Hou Yip when directly training on real data. We use a Generative Adversarial Network to obtain a (UCL) suitable dataset for training Convolutional Neural Network classifiers to detect and locate planets across a wide range of SNRs. Tested on artificial data, our detectors exhibit good predictive performance and robustness across SNRs. To demonstrate the limits of the detectors, we provide maps of the precision and recall of the model per pixel of the input image. On real data, the models can re-confirm bright source detections.

Observation and Data Reduction No. Title Abstract Time Name (Affiliation) P6-01 Data Processing and Through careful data processing, observations using the Gemini Planet Imager’s IFS and Calibrations for the polarimeter have yielded insights into exoplanetary systems and circumstellar disks. We present Gemini Planet Imager the latest methods in calibrating GPI data to yield astrophysically unbiased measurements at Exoplanet Survey high contrast. In particular, we present improvements in the data pipeline related to photometric calibration using the satellite spots, precise astrometric calibration and handling of subtle systematic offsets, and reduction of instrumental polarization signatures in some datasets. A Marshall Perrin sophisticated automated data processing system has managed consistent reductions of the entire (Space Telescope GPI Exoplanet Survey data set, including application of advanced PSF subtraction and forward Science Institute) modeling capabilities, to yield systematic measurements suitable for measurements of exoplanet demographics, as well as data mining investigations of performance factors affecting achieved contrast. At the conclusion of GPI Exoplanet Survey observations, GPI is a well-understood and carefully calibrated system. P6-02 A highly-automated We present a highly-automated end-to-end pipeline to reduce VLT/SPHERE-IRDIS end-to-end pipeline to polarimetric data called IRDAP (IRDIS Data reduction for Accurate Polarimetry) which is

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reduce VLT/SPHERE- publicly available at https://irdap.readthedocs.io. IRDAP’s core feature is the correction of IRDIS polarimetric instrumental polarization effects based on our fully validated Mueller matrix model describing data the instrument and telescope. With this correction IRDAP reaches a polarimetric accuracy of <0.1% in the degree of linear polarization and an accuracy of a few degrees in angle of linear polarization in Y-, J-, H- and Ks-band. Data taken with the narrowband filters can also be Rob van Holstein reduced, although with a somewhat lower accuracy. IRDAP handles both field- and pupil- (Leiden Observatory) tracking data, and for the latter can additionally perform angular differential imaging (ADI). Reducing data with IRDAP is very straightforward and does not require the user to do any coding. IRDAP is written in Python 3, but is simply run from a terminal with only a few commands and using a simple configuration file. For an average sized data set and using a modern computer, IRDAP performs a complete data reduction from raw data to final data products within a few minutes. IRDAP yields a multitude of improvements for observations of circumstellar disks: it enables us to accurately study the morphology of disks, measure non- azimuthal polarization and determine scattering phase functions. Because IRDAP discerns instrumental polarization from stellar polarization, it is a vital tool for accurate radiative transfer modeling of disks and enables the detection of unresolved (inner) disks and the measurement of the polarization of substellar companions and exoplanets. For pupil-tracking data IRDAP can detect companions and circumstellar disks in total intensity, enabling us to immediately retrieve the degree of linear polarization. Finally, IRDAP enables accurate data reduction for targets that cannot be reduced with conventional data-reduction methods such as solar system objects. P6-03 Comparison between The extensive study of beta Pictoris has evidenced discrepancies between SPHERE and GPI SPHERE and GPI astrometries. We will present a study performed to understand the origin of these discrepancies. astrometries

Anne-Marie LAGRANGE (IPAG CNRS) P6-04 High-contrast Imaging Image rotation and subtraction (IRS) is a high contrast imaging technique to suppress the technique combining speckle noises in exoplanets direct imaging. The calibration of speckle noises in IRS is based on IRS and ADI the 180 degree rotated images. Since IRS does not suffer from planet self-subtraction, it has higher SNR for the planet in the inner region around the star. In this work, we develop an Gang Zhao optimization algorithm combining the IRS and ADI method. During the optimizing, an (Nanjing Institute of coefficient is introduced to control the weights of the IRS and ADI. We make a comparison of Astronomical Optics the signal-to-noise ratio (S/N) achieved by different algorithms and find that the performance &Technology) can be improved by using our IRS-ADI hybrid high contrast imaging technique. P6-05 New algorithms to Direct imaging is a powerful technique to detect and characterize giant planets at tens of au improve the quality of from the central star, providing valuable constraints on the formation mechanism. The “angular NACO coronagraphic differential imaging” technique has proven to be successful to detect such planets at different images. wavelengths in the near-infrared. One of the main challenge when observing in the L' band for instance is the significant contribution of the thermal background emission from the sky, leading to tens of thousands of frame for a single object. The second challenge lies in the use of Nicolas Ignacio Godoy a coronagraph, which can, for some instruments, prevent to know the location of the star behind Barraza the optical components. The NACO-ISPY (Imaging Survey for Planets around Young stars) is a (Instituto de Fisica y VLT/NACO survey that observes young stars looking for sub-stellar companions where the Astronomia, Facultad de typical number of frames per target varies between 20.000 to 40.000 in a single observation. In Ciencias, Universidad de this work I will present a novel technique to refine the centering of NACO-ISPY observations Valparaiso) and a systematic study about the impact of frame selection on the data reduction process. Both techniques (centering and frame selection) are crucial to improve the final contrast of the images and possibly detect faint sources. This work incorporates the idea of automatic frame selection and the quantification of its improvements on the reduced images. P6-06 Studying giant planet Giant planets are thought to form at large orbital separations (~5-20 au), which is why direct formation with Fourier imaging is crucial to study their formation process. However, most of the early direct detections plane imaging of young giant proto-planets have emerged to be light scattering features of morphologically techniques complex transitional disks instead. Hence, studying forming planets remains elusive and planet formation theories remain speculative. However, the recent and unique example of PDS 70 shows that young giant proto-planets are Jens Kammerer particularly bright. Nevertheless, planet formation at ~20 au (PDS 70 b) and ~35 au (PDS 70 c) (European Southern is very rare and the nearest associations of young stars are>100 pc away, where resolving solar Observatory/ANU) system scales is challenging.

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In this talk, we present our recent work (Kammerer et al. 2019) on kernel phase imaging below the diffraction limit of the VLT which gives access to such scales (5-20 au or 40-140 mas) in the nearest star-forming regions. We introduce novel techniques for high-resolution, high- contrast Fourier plane image analysis that are publicly available in our modular pipeline. Moreover, we show preliminary results from our survey of Taurus targets and report on the extensive, still poorly understood systematic errors in Fourier plane imaging (NRM/kernel phase) and optical/near-infrared interferometry. Finally, we present our ongoing work to improve the dynamic range in interferometric detection of faint companions by taking into account the correlated errors. Our preliminary work results are applied to VLTI/GRAVITY data. P6-07 Numerical Self-calibration is an interferometric tool that extracts from the data observables that are robust Investigations of to individual antenna errors. Kernel phase-amplitude methods generalize interferometric self- Coronagraphic Self- calibration to full aperture optical telescopes in a linearized low wavefront aberration regime. Calibration While coronagraphs help reduce the amount of unwanted starlight in the image, self-calibration has not previously been extended to coronagraphic instruments involving more than just a pupil plane mask. We numerically investigate prospects for self-calibration with a focal plane mask Yinzi Xin coronagraph. We model a Lyot coronagraph and find a regime dominated by a linear term and a (MIT) regime dominated by a quadratic term, depending on the angular separation and level of wavefront aberration. Transfer matrices are numerically built for each regime, their kernel spaces are obtained, and self-calibrated observables are extracted. Using the corresponding kernel, we measure a reduction of more than a factor of 5 on the effect of speckles both at 4 lambda/D in the linear regime and at 11 lambda/D in the quadratic regime. We discuss prospects for applying self-calibration with current coronagraph designs and for analysis of archival coronagraphic data. P6-08 Exploring the limits of The Medium Resolution Spectrograph (MRS) on the Mid-Infrared Instrument (MIRI) of JWST directly imaging is an integral field spectrograph with a spatial resolution of 0.3''-1’’ and providing a spectral exoplanets with the resolution of 1500 to 3000 in the 5-28 micron wavelength range. In preparation of the first GO Medium Resolution cycle and the MIRI GTO program on exoplanets and brown dwarfs we investigated the Imaging Spectrograph capability of the MRS to directly image exoplanets and attempt extracting a spectrum of their on JWST MIRI atmospheres. Using the MIRI Simulator and instrument specific knowledge, we created simulated observations and apply our reduction pipeline, which, in order to remove the stellar PSF, takes advantage of both spatial and spectral information. In this talk I will summarise our Polychronis Patapis findings and discuss the limits of a realistic parameter space for exoplanets that could be (ETH Zurich) observed with the MRS. P6-09 A vector Apodising Planetary rotation and atmospheric features, such as giant storms and hurricanes, give rise to Phase Plate view of an photometric variability in exoplanet atmospheres. Measuring these variations is challenging for exoplanet atmosphere ground-based coronagraphic imaging due to the lack of a reference source for photometric calibration. Yet ground-based telescopes provide the angular resolution necessary to detect exoplanets residing at small angular separations. I will present results from two full nights of Ben Sutlieff direct time series monitoring of HR 2562, an F5V star with a known planetary-mass companion, (Anton Pannekoek obtained using the Vector Apodising Phase Plate (vAPP) coronagraph at the 6.5-m Magellan Institute, University of Clay Telescope. These observations were designed to test the ability of ground-based Amsterdam) instruments to create planetary light curves. Unlike traditional focal-plane coronagraphs, the vAPP coronagraph offers both deep suppression of stellar light and an unsaturated stellar reference, thus enabling differential photometry with expected precision at the 1% level. Curiously however, we do not detect HR2562 b at its expected 10-4 contrast, indicating that the companion is anomalously faint at 3.9 microns based on measurements at shorter wavelengths. Nonetheless, we are able to demonstrate that vAPPs can achieve sufficiently deep speckle suppression such that light curve measurements are possible for systems with more favourable star-planet contrast ratios. P6-10 Atmospheric retrievals The field of exoplanetary spectroscopy is as fast moving as it is new. Analysing currently of directly imaged available observations of exoplanetary atmospheres often invoke large and correlated parameter planets using TauREx3 spaces that can be difficult to map or constrain. This is particularly true for inverse retrievals of and deep learning atmospheres. In this conference I will present the new TauREx3 framework which is a current state-of-the-art retrieval suite for exoplanet atmospheres. TauREx3 builds on the heritage of TauREx2 software Ingo Waldmann which was extensively used for transit and eclipse spectroscopy of exoplanets in the past. (University College TauREx3 has been built from scratch to optimise speed, model complexity and usability. To London (UCL)) fully sample the Bayesian likelihood space of the retrieval while maintaining model complexity (i.e. slower forward models), we use likelihood predictive deep learning to speed up

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convergence without loosing accuracy. At the Spirit of Lyot conference, we will demonstrate spectroscopic retrievals of directly imaged planets using TauREx3. P6-11 Refining exoplanet Exoplanet atmospheric retrievals —inferring the atmospheric properties of extrasolar planets— atmospheric retrievals consist of fitting atmospheric models to the exoplanet’s observed emission or transmission with information- spectrum, obtained via either direct imaging or the transit method. The problem is a challenging theoretic methods one for multiple reasons including —among others — the limited ground truth, the low signal- to-noise-ratio, the huge parameter space and the presence of degeneracies (equivalent solutions). Nikolaos Nikolaou In this work we propose the use of information-theoretic machinery to alleviate these issues and (University College improve the speed and quality of the resulting retrievals. We will discuss the use of measures London) based on mutual information to perform (i) feature selection on the spectrum (identify which combinations of wavelengths are the most informative with respect to the parameters to be retrieved) and (ii) model selection on candidate retrievals (identify which of the candidate atmospheric retrievals is offering the best fit to the observed data while being characterised by the simplest underlying model, in the information-theoretic sense). The ideas discussed in this work can directly be applied to obtaining fast initial solutions to atmospheric retrievals, improving their quality by removing redundant or irrelevant spectral features, by allowing us to choose a more appropriate wavelength resolution or by selecting the most robust among multiple candidate retrievals. Beyond this, the very same analysis can extend to comparing and combining observations from different instruments and (applied to a high-resolution spectrum) to informing the design of future space missions.

Combination of Indirect and Direct Exoplanet Observation No. Title Abstract Time Name (Affiliation) P7-01 Combining high We present recently published results from a joint analysis of high contrast imaging (HCI) and contrast imaging and radial velocity (RV) data to constrain the planetary architectures of 6 nearby (<6 pc) stars: radial velocities to Ceti, Kapteyn's star, AX Mic, 40 Eri, HD 36395, and HD 42581. Combining information from constrain the planetary the complementary detection methods of HCI and RV provides strong constraints on the 𝜏𝜏 architecture of nearby existence of planetary systems because these methods are sensitive to companions in different stars regions of the mass and semi-major axis parameter space. Our analysis is based on archival VLT/NACO HCI data at L’ band (3.8 µm) and RV data from HARPS, Keck/HIRES, and CORALIE. The archival NACO data were fully re-analyzed using the state-of-the-art direct Anna Boehle imaging pipeline PynPoint, which uses Principal Component Analysis to model and subtract the (ETH Zurich) stellar point spread function. The HCI mass limits reach 5 - 20 Jupiter masses in the background-limited regime, depending on the age of the star. We find that the HCI data add significant information to the RV constraints, increasing the completeness for certain companion masses/semi-major axes by up to 68 - 99% for 4 of the 6 stars in our sample, and by up to 1 - 13% for the remaining stars. The improvements are strongest for intermediate semi- major axes (15 - 40 AU), corresponding to the semi-major axes of the ice giants in our own solar system. Applying these methods to combine HCI and RV information systematically to nearby stars will help us prioritize target lists for future missions and instruments (e.g., VLT/ERIS, ELT/METIS, Habex and LUVOIR). P7-02 Results from the Beta Beta Pictoris b is the only extrasolar gas giant planet that has been directly imaged and has an Pictoris b Hill Sphere edge-on orbit that causes the planet's Hill sphere to transit approximately every 22 years. Based Transit Campaign on multi-epoch direct imaging observations from the Gemini Planet Imager, the Hill sphere began transiting in April 2017, with closest approach to within 20% of the 1.2au Hill sphere radius in August 2017. We present the results from the combined space and ground based Matthew Kenworthy photometric campaigns that cover the entirety of the Hill sphere transit during 2017 and the first (Leiden Observatory) half of 2018, to search for signs of circumplanetary dust and rings. These include a dedicated monitoring instrument in South Africa and Australia (the bRing project), the BRITE- Constellation nanosatellites, two telescopes in Antarctica (ASTEP and AST3) and HST/COS data. P7-03 Looking for Planets in Space-based exoplanet direct imaging promises a wealth of new discoveries, as well as new all the Right Places: challenges, including extremely strict limits on instrument availability, which will require Target Selection for optimization of all observations. A major part of this optimization is the selection of appropriate Direct Imaging targets, which fall into three classes: stars with no current evidence of companions, stars with known companions that have some chance of being imaged, and stars with known companions that cannot be imaged, but which can can have additional, imageable companions on stable

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Dmitry Savransky orbits. Using the WFIRST coronagraphic instrument as a motivating example, we will discuss (Cornell University) each of these three cases, and demonstrate tools and techniques for prioritizing targets in each category. These include target completeness, target depth of search, known planet completeness, and unknown stable companion completeness. P7-04 The 2019 WFIRST The 2019 WFIRST Exoplanet Imaging Data Challenge (www.exoplanetdatachallenge.com) will Exoplanet Imaging be launched in mid October just prior to this Spirit of Lyot Conference (Hack Dat on October Data Challenge 20th in Tokyo). It is a unique opportunity for exoplanet scientists of all backgrounds and experience levels to get acquainted with realistic WFIRST CGI simulated data. Candidate teams will be invited to recover the components of an exoplanetary system from two to six imaging Julien H. Girard epochs throughout the mission life time with with Hybrid-Lyot Coronagraph (HLC) and Star (Space Telescope Shade (SS) coronagraph. CGI’s contrast regimes at 10-8 to 10-9 is unlike what the community is Science Institute used to from the ground. To perform accurate orbital fitting with a few imaging epochs, we will (STScI)) provide the corresponding simulated radial velocity data. Possible hurdles to overcome are contamination sources (stellar, extragalactic, exozodiacal light, etc). Do you want to know what it feels like to directly image a Neptune-mass planet in reflected light? Then, join our data challenge! It is an excellent way to get involved with the intricacies of the first spaceborne high contrast exoplanet imaging mission, as a pathfinder to future flagship missions.

Future Plan and Facility No. Title Abstract Time Name (Affiliation) P8-01 An Overview of the We have proposed an instrument, the Planetary Systems Imager, that has recently been TMT Planetary identified as a priority for the Thirty Meter Telescope. Our aims are to detect and characterize Systems Imager exoplanets in reflected light and thermal emission. I will briefly summarize the science goals of this instrument and its broad range of capabilities, and will give an overview of the instrument architecture. I will also summarize the activities during the conceptual design of the project. Michael Fitzgerald One significant activity in support of this conceptual design study is the development and use of (Infrared Laboratory) a simulation toolchain. I will describe the components of this toolchain and how they are supporting different activities in the project. I will describe the future development plans for the instrument, including strategies for deployment on the telescope. P8-02 The game-changing METIS, the mid-infrared ELT imager and spectrograph, is one of the three first-generation promises of instruments of the Extremely Large Telescope. It recently passed its preliminary design review, ELT/METIS for and is expected to see first light in 2027. Specifically designed to deliver high-contrast imaging exoplanet imaging capabilities, METIS features advanced coronagraphic concepts such as a ring-apodized vortex coronagraph and an apodizing phase plate. It also comprises a high-resolution (R=100,000) integral field spectrograph covering wavelengths from 3 to 5 µm, which can be combined with Olivier Absil the coronagraphic observing modes. Using the full resolving power of the ELT thanks to a high- (University of Liege) performance adaptive optics module, METIS promises to reach game-changing performance in the field of exoplanet imaging. In this talk, I will review the design and expected performance of METIS high-contrast imaging modes. I will then describe some of the most appealing science cases that will be addressed by METIS in the field of exoplanet imaging, including the possible discovery of temperate rocky planets in the alpha Centauri system, the high-spectral resolution study of Proxima b, or the spectral characterization of exoplanets discovered by radial velocities or astrometry (Gaia follow-up). I will conclude this talk by decribing our plans to deploy machine learning techniques in the operation and data analysis of the METIS high contrast imaging modes. P8-03 Exoplanet direct High-contrast imaging is a unique method to probe the outer regions of young exoplanetary detection and systems, and thus gives insight into the formation, composition and evolution of young giant characterization with exoplanets. Current high-contrast instruments provide spectro-imaging capabilities at low the ELT/HARMONI spectral resolution (R = 30-100) that allow the detection and first-order characterization integral field (temperature, surface gravity) of giant planets, but significantly higher resolutions would be spectrograph required for more detailed estimations (abundances, orbital and rotational velocities). The next generation of instruments on extremely large telescopes (ELTs) will be ideal for this task. HARMONI will be one of the first-light instruments mounted on ESO’s ELT planned for 2025. Mathis Houlle It is a medium-resolution (up to R = 17,000) integral field spectrograph in the optical and the (Laboratoire near-infrared, which will be equipped with a single-conjugated adaptive optics system to reach d'Astrophysique de the diffraction limit of the ELT in the H- and K-bands. For direct exoplanet detection and Marseille (LAM)) characterization, HARMONI will include a high-contrast module that will provide unprecedented contrast limits at separations between 50 and 400 mas, i.e. down to 1 AU for a

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star at 20 pc. Exoplanet detection will be further facilitated by the medium spectral resolution of HARMONI, which allows detection based on the expected planetary spectral features. In this talk, we will present an estimation of HARMONI capabilities for exoplanet detection, based on realistic simulated data for the high-contrast mode and new analysis tools exploiting the spectral information, such as “molecule mapping” techniques (e.g. Hoeijmakers et al. 2018). We will compare these new detection limits to classical high-contrast imaging techniques, based on angular differential imaging, to demonstrate the potential of medium-resolution spectroscopy for exoplanet detection. Finally, we will show estimations of HARMONI performances for physical, orbital and atmospheric characterization of exoplanets. P8-04 Exoplanet Sciences The starshade is a powerful tool for direct imaging of exoplanets. Using a starshade to suppress with Starshade unwanted starlight, the contrast and inner working angle are largely decoupled from the telescope aperture size, and high throughput and broad wavelength bandpass are achievable. I will review important exoplanet science applications enabled by direct imaging exoplanet Renyu Hu missions with a starshade, using the Starshade Rendezvous Mission (SRM) concept as the (Jet Propulsion baseline. The SRM consists of a starshade flying with WFIRST and using its coronagraph Laboratory, California instrument to perform space-based direct imaging. The SRM will enable “deep dive” searches Institute of Technology) of planetary systems in our nearest neighbor stars, with the potential to detect and characterize Earth-like planets in the habitable zone around Sun-like stars. The SRM will also obtain reflected light spectra of known giant planets at wide orbital separations from their host stars. I will present a new spectral retrieval method that self-consistently couple cloud formation with the rainout of cloud-forming gases, and show that detail characterization of the atmospheric components, e.g., CH4, NH3, H2O, and clouds, is possible with the reflected light spectra. Between Earth-sized planets and giant planets, a diversity of planets from various types of super-Earths to mini-Neptunes could be found. I will discuss this greatly expanded search space, and how it represents a uniquely powerful opportunity to discover and explore a panoply of fascinating and potentially habitable planets in 2020 – 2030 and beyond. P8-05 A Standard comparison The HabEx and LUVOIR concept studies, contributed to the 2020 Astrophysics Decadal Survey of exoplanet yield for as potential future large space telescopes, aim to directly image and spectrally characterize the LUVOIR and potentially habitable exoplanets. A common comparison of exo-earth yield was performed by HabEx Concept Studies NASA’s Exoplanet Exploration Program (ExEP) Standard Definition and Evaluation Team (SDET). The SDET was chartered to perform an unbiased comparison of the exoplanet yields using common inputs, assumptions, analysis methods, and metrics. For astrophysical inputs, the Rhonda Morgan SDET uses the exozodi distribution measured by the LBTI HOSTS survey, the orbit fitting (NASA/JPL) heuristic developed by Nielsen et al., and the SAG13 occurrence rates as modified by Dulz for long period and high mass planets. The yield analysis employed two simulation codes: AYO by Stark and EXOSIMS by Savransky et al. The AYO code utilizes static time allocation to determine the cumulative completeness (probability of detection), setting an upper bound on yield performance. EXOSIMS is a design reference mission simulator that synthesizes planets around stars, schedules and renders observations based on sun constraints, and responds dynamically in the schedule to observations during the simulation. EXOSIMS provides insight into derating of yield due to realistic schedule challenges. HabEx is evaluated for the 4m hybrid starshade and coronagraph architecture, the 4m coronagraph only architecture, and the 4 m starshade only architecture. LUVOIR is evaluated for the 9 m architecture of their final report. Yield analysis shows that both concepts can directly image and spectrally characterize earth-like planets in the habitable zone and that each concept has complementary strengths. P8-06 The NASA/NSF Following the recommendation of the U.S. National Academy of Sciences' Exoplanet Science Extreme Precision Strategy Report, NASA and NSF have formed a Working Group on Extreme Precision Radial Radial Velocity Velocity measurements. Radial velocity measurements provide essential mass, orbit, and Initiative demographic information that supports studies of both transiting and directly imaged planets. They are currently limited by variations in the stellar photosphere, instrumental stability and calibration, and spectral contamination from telluric lines. Progress will require new Karl Stapelfeldt instruments installed on large telescopes, substantial allocations of observing time, advanced (Jet Propulsion statistical methods for data analysis informed by theoretical modeling, and collaboration Laboratory, California between observers, instrument builders, stellar astrophysicists, heliophysicists, and statisticians. Institute of Technology) The Working Group is tasked to recommend an investment strategy that would advance the state of the art to the point where Earth-like exoplanets can be detected orbiting Sun-like stars. Upon receipt of the Working Group's report in spring 2020, U.S. Federal Agencies will then consider if, when, and how to implement that strategy. This poster is a progress report on Working Group activities through summer 2019.

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P8-07 The NASA Exoplanet The goals of the NASA Exoplanet Exploration Program (ExEP) are to discover planets around Exploration Program other stars, characterize their properties, and identify candidates that could harbor life. Toward Science Gap List those goals, the Program maintains a Science Gap List (SGL) as a guide to decisions on current and future investments. Broadly speaking, a Program science gap is a research area where additional work would meaningfully enhance the science return of current or past exoplanet Karl Stapelfeldt missions, or would provide precursor information needed to carry out future exoplanet missions. (Jet Propulsion NASA's portfolio of current and future missions is defined in the NASA Astrophysics Laboratory, California Implementation Plan, and flows from U.S. community policy documents such as the Decadal Institute of Technology) Surveys. Each gap is described in terms of the capability needed, the capability today, and the status of efforts in NASA and the broader community to close the gap. Rather than capturing all the scientifically interesting areas of exoplanet research, the focus of the SGL is to identify and crisply define work needed to advance NASA's exoplanet exploration goals. The ExEP SGL is not meant to provide strategic community guidance on par with a National Academies report (e.g. Decadal Survey, Exoplanet Science Strategy, etc.), but to provide tactical guidance for program management within the ever-shifting landscape of NASA missions and mission studies. Funding sources outside of NASA ExEP are encouraged to refer to the SGL as they make judgements on whether to align the work they support with NASA’s Exoplanet Exploration goals. This poster presents the gap list and strongly encourages comments and suggestions from the community.

Other No. Title Abstract Time Name (Affiliation) P9-01 Chasing free-floating The free-floating planet (FFP) hunting is relying on the microlensing observation, and the mass planet from a parallax and distance are only what we can know from the observed data. For a stellar lens microlensing observation of a event, the additional direct imaging observation sometimes works to identify the lens motion, microlensing event but the method is not applicable to FFP lenses. Therefore, we considered the approach of the FFP motion identification from the microlensing parallax observation. The shortness of the FFP event takes advantage of the parallax observation between the Earth's observer and next Makiko Ban generational space-based surveys such as Euclid and WFIRST by neglecting the parallax (National Astronomical influence made by the observers' own motion. In this research, we assumed the parallax Observatory of Japan) observation between Euclid and Earth's observer and run the simulation to yield light curves they detect by varying the direction of the relative proper motion of the lens-- the incident angle of the lens passing the source on the sky reference frame. We found there is a preference of the incident angle to yield a large difference between light curves detected in parallax. It is expectable to narrow down the candidates of lens proper motion from the light curves and the incident angle distribution map adjusted for the event. P9-02 High contrast shock We found multiple shock emission features around VV CrA binary system with spectral emission structures mapping technique with IGRINS/Gemini(South), which is a high spectral resolution around VV CrA in spectrograph (R~ 45,000) covering whole H and K bands simultaneously. We did slit scanning datacube data achieved with 12 transverse slits against the binary direction (PA=44 degree) and constructed datacubes by high spectral for multiple H_2 and [Fe II] emission lines. The FoV covers ~4''x 5''. The velocity resolution is resolution (R ~45000) ~ 5-7 km/s. After continuum subtraction, the high-contrast channel map images of H2 and [Fe II] emissions reveal multiple and complex emission structures around VV CrA for the first time. H2 1-0 S(1) emission shows three distinct knot structures: SE knot with Vr ~ -14 km/s, SE- Tae-Soo Pyo extension from IRC (IR companion) with Vr ~ -7 km/s, NW knot from primary with Vr ~ -3 (Subaru Telescope/ km/s. All three H2 knots have ~ 20 km/s velocity width. IRC and primary stars also show H2 NAOJ) emissions, which show ~ 4 km/s deviation in peak velocity each other. [Fe II] 1. 644 micron emission shows very high velocity with Vr ~ 144 km/s at a knot located east side of the primary and Vr ~ 197 km/s at south-west and north side surrounding the primary. Even any conventional narrow band filter imaging could not show these features due to low contrast by dilution with continuum emission. Our data show multiple jets signature from the binary or shocked environment around circumbinary or circumstellar disks. P9-03 Vegetation red edge on High contrast imaging of planetary system by masking out the light from central star was water planets around originated from Bernard Lyot’s effort for developing a perfect coronagraph in 1930’s. Direct M-dwarfs imaging of habitable exoplanets is a promising goal in the next decade, though detecting biosignature on the exoplanets is more ambitious goal. While the all organisms have some interaction with planetary environment, most of biological activities are much smaller than Kenji Takizawa geological and meteorological activities. Land plants on Earth shows large gap in reflectance

65 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

(Astrobiology Center) between visible light and infrared radiation because of selective absorption of visible light for photosynthesis. Photosynthesis is a fundamental biological reaction that converts naturally abundant light energy to biologically available chemical energy. If an exoplanet has a developed land vegetation as on Earth, red-edge might be detectable by a telescopic observation. Even on the water planets that are completely covered by deep ocean, red-edge could be detectable if there are floating aquatic vegetation. On the current Earth, floating plants inhabit relatively small-scale wetlands or shallow water. In the middle Eocene epoch, though, the arctic ocean could be covered by freshwater fern Azolla. In the evolution of life on Earth, sponge-leaf structure of plants had evolved after land adaptation of water plants. To expect observing red- edge on water planets, direct evolutionary pathway from aquatic plants to floating plants has to be assumed.

66 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Authors of presentations

Exoplanet Imaging

Characterizing Directly Imaged Exoplanets

Quinn M Konopacky (University of California)

The Next Generation of Exoplanet Direct Imaging with Extreme Adaptive Optics

Thayne Currie (NASA-Ames Research Center) and Olivier Guyon

Characterizing a directly-imaged planet Kappa And b with SCExAO

Taichi Uyama (Caltech/IPAC, NASA Exoplanet Science Institute), Thayne Currie (NASA AMES), Yasunori Hori (ABC), Robert DeRosa (Stanford University), Kyle Mede (the University of Tokyo), and SCExAO team

Exoplanet Direct Imaging Surveys: the statistical picture

Beth Alison Biller (University of Edinburgh)

Young Suns Exoplanet Survey (YSES) reveals planets, brown dwarfs, and disks in Sco-Cen

Alexander Julian Bohn (Leiden University), Matthew A. Kenworthy (Leiden University), Christian Ginski (University of Amsterdam), Jozua de Boer (Leiden University), Christoph U. Keller (Leiden University), Eric E. Mamajek (California Institute of Technology, University of Rochester), Tiffany Meshkat (California Institute of Technology), Mark J. Pecaut (Rockhurst University), Maddalena Reggiani (KU Leuven), Frans Snik (Leiden University)

Planets and protoplanets revealed by the molecular mapping technique

Mickael Bonnefoy (Institut de Planetologie et d'Astrophysique de Grenoble), A.-M. Lagrange, G. Chauvin, J. Rameau, B. Charnay, S. Petrus, A. Boccaletti, A. Carlotti, P. Delorme, J. Hoeijmakers, M. Keppler, M. Benisty, T. Henning, and M. Langlois

First constraints on the population of young giant exoplanets from the SPHERE infrared survey for exoplanets (SHINE)

Arthur Vigan (Laboratoire d'Astrophysique de Marseille / CNRS), Michael Meyer (University of Michigan) Beth Biller (Observatory of Edinburgh) Clemence Fontanive (Observatory of Edinburgh) Markus Feldt (MPIA) Mariangela Bonavita (Observatory of Edinburgh) SHINE consortium

Status of the SPHERE/SHINE survey: From the observations to the exoplanet detection performances

Maud Langlois (CNRS/CRAL), and the SPHERE/SHINE consortium 67 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

The VIBES Exoplanet Survey with SPHERE

Natalia Engler (ETH Zurich Institut for Particle Physics and Astrophysics), and VIBES team

The new COPAINS tool for target selection and orbital characterisation of direct imaging systems

Clemence Fontanive (University of Bern), Beth Biller (University of Edinburgh), Mariangela Bonavita (University of Edinburgh), Koraljka Muzic (Universidade de Lisboa)

Detailed Monitoring of the HR 8799 Planets

Jason J. Wang (Caltech), Peter Gao (UC Berkeley), Sylvestre Lacour (Observatoire de Paris), Jeff Chilcote (Notre Dame), Mathias Nowak (Observatoire de Paris), the SCExAO Team, the GRAVITY Collaboration

Spectral characterization of newly detected young substellar binaries with SINFONI

Per Calissendorff (Stockholm University), Markus Janson (Stockholm University), Ruben Asensio- Torres (Stockholm University), Rainer Koehler (Leiden University)

MIRACLES: an atmospheric characterization survey of planetary and substellar companions at 4-5 micron

Tomas Stolker (ETH Zurich), Sascha Quanz (ETH Zurich), Paul Molliere (Leiden University), Michael Meyer (University of Michigan), Jonas Kuhn (University of Bern), Kamen Todorov (University of Amsterdam), Anthony Cheetham (MPIA)

Active minimization of non-common path aberrations using a self-coherent camera for imaging exoplanetary systems

Garima Singh (LESIA, Observatory of Paris), Raphael Galicher (LESIA), Pierre Baudoz (LESIA) Olivier Dupuis (LESIA), Manuel Ortiz (LESIA), Axel Potier (LESIA), Simone Thijs (LESIA) and Elsa Huby (LESIA)

Moderate Resolution Spectroscopy of Directly Imaged Exoplanets

Kielan Kathryn Wilcomb (UC San Diego), Quinn Konopacky (UC San Diego), Travis Barman (University of Arizona), Christopher Theissen (UC San Diego), Laci Brock (University of Arizona), Bruce Macintosh (Stanford), Jean-Baptiste Ruffio (Stanford), Christian Marois (NRC-Herzberg)

The WFIRST Coronagraph telescope simulator: Building a coronagraph calibrator

Eduardo Bendek (NASA Jet Propulsion Laboratory), Hong Tang (JPL), Brian Kern (JPL), Gary Kuan (JPL), Keith Patterson (JPL), James Wu (JPL)

Deformable Mirrors Controller Architectures for High-Contrast Imaging Overview

Camilo Mejia Prada (JPL), Eduardo Bendek, Garreth Ruane

68 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Moderate Resolution Spectroscopy of Directly Imaged Exoplanets

Kielan Kathryn Wilcomb (UC San Diego), Quinn Konopacky (UC San Diego), Travis Barman (University of Arizona), Christopher Theissen (UC San Diego), Laci Brock (University of Arizona), Bruce Macintosh (Stanford), Jean-Baptiste Ruffio (Stanford), Christian Marois (NRC-Herzberg)

The WFIRST Coronagraph telescope simulator: Building a coronagraph calibrator

Eduardo Bendek (NASA Jet Propulsion Laboratory), Hong Tang (JPL), Brian Kern (JPL), Gary Kuan (JPL), Keith Patterson (JPL), James Wu (JPL)

Deformable Mirrors Controller Architectures for High-Contrast Imaging Overview

Camilo Mejia Prada (JPL), Eduardo Bendek, Garreth Ruane

Overview of the WFIRST Coronagraph Instrument and exoplanet science

Vanessa Bailey (Jet Propulsion Lab), WFIRST CGI instrument and science teams

First Light Results from the Keck Planet Imager and Characterizer

Nemanja Jovanovic (Caltech), Jacques-Robert Delorme (Caltech) Charlotte Bond (IfA) Dimitri Mawet (Caltech) Sylvain Cetre (Keck) Daniel Echeverri (Caltech) Scott Lilley (Keck) Kent Wallace (JPL) Randy Bartos (JPL) Jason Wang (Caltech) Jacklyn Pezzato (Caltech) Sam Ragland (Keck) Peter Wizinowich (Keck) Marck Chun (IfA) Ed Wetherell (Keck) Michael Fitzgerald (UCLA) Eric Wang (UCLA) Emily Martin (UCLA) Eric Warmbier (IfA) Charles Lockhart (IfA) Don Hall (IfA) Garreth Ruane (JPL) Andy Skemer (UCSC) Jennah Colborn (Caltech)

The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10-100 AU

Eric L. Nielsen (KIPAC/Stanford), Robert J. De Rosa (Stanford), Bruce Macintosh (Stanford), Jason J. Wang (Berkeley, Caltech), Jean-Baptiste Ruffio (Stanford), Eugene Chiang (Berkeley), Mark S. Marley (NASA Ames), Didier Saumon (Los Alamos), Dmitry Savransky (Cornell), and the Gemini Planet Imager Exoplanet Survey team

First Constraints on the 3D Angular Momentum Architecture of a Planetary System

Marta Levesque Bryan (UC Berkeley), Brendan Bowler (UT Austin), Sarah Blunt (Caltech), Henry Ngo (NRC Herzberg), Caroline Morley (UT Austin), Dimitri Mawet (Caltech)

VISIR/NEAR, a 100-hour direct imaging search for low-mass planets in alpha Centauri

Markus Kasper (ESO), the NEAR team

Thermal-Infrared Integral Field Spectroscopy of Planets and Protoplanets

Jordan Michael Stone (University of Arizona), LBTI team, NALES team, vAPP team

69 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Imaging gap-carving, accreting protoplanets with MUSE

Julien H Girard (Space Telescope Science Institute (STScI)), Sebastiaan Haffert (Leiden Observatory) Jos de Boer (Leiden Observatory) Rob van Holstein (Leiden Observatory) Alex Bohn (Leiden Observatory) Ignas Snellen (Leiden Observatory) Jarle Brinchmann (Leiden Observatory) Christoph Keller (Leiden Observatory) Roland Bacon (Lyon Observatory) Peter Zeidler (STScI) Jaehan Bae (Carnegie DTM)

Near-visual integral-field spectroscopy of the circumbinary planet / brown dwarf 2M0103(AB)b with the new Narrow Field Mode on MUSE

Simon Christoffer Eriksson (Stockholm University), Markus Janson (Stockholm University), Ruben Ascensio-Torres (Stockholm University)

BEAST: The B-star Exoplanet Abundance Study

Markus Janson (Stockholm University), The BEAST collaboration

Gemini Planet Imager Spectroscopy of the Reddest Known Substellar Companion HD206893 B

Kimberly Ward Duong (Amherst College/Five College Astronomy Department), Jenny Patience (ASU), Kate Follette (Amherst College), Robert De Rosa (Stanford), Julien Rameau (IPAG), Eric Nielsen (Stanford), Mark Marley (NASA Ames), Abhijith Rajan (STScI), Alexandra Greenbaum (U. Michigan), and the GPIES Team

A tentative first direct detection of a circumplanetary disk

Tobias O. B. Schmidt (Hamburg Observatory), SPHERE consortium / SHINE and disk team

Searching for Additional Outer Planets Around HR8799

William Raal Thompson (University of Victoria), Christian Marois (NRC HAA) and Quinn Konopacky (UC San Diego)

Unveiling a population of sub-stellar binary companions in a young cluster: HST survey of the Orion Nebula Cluster in the H2O

Giovanni Maria Strampelli (STScI), Jonathan Aguilar (JHU), Laurent Pueyo (STScI), Antonio Aparicio (ULL/IAC), Mario Gennaro (STScI), Leonardo Ubeda (STScI) and Massimo Robberto (STScI)

Detecting distant, sub-Jovian planets in scattered light through their circumplanetary debris disks

Daniel Tamayo (Princeton University), Loic Nassif-Lachapelle (University of Toronto)

Imaging Temperate Exoplanets

Andy Skemer (UC Santa Cruz), TBD

70 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

The Bright Future of Protoplanet Direct Imaging - Lessons Learned from the First Generation Magellan Giant Accreting

Dirk Maarten van Dam (Leiden Observatory), Christian Ginski (Anton Pannekoek Instituut), Matthew Kenworthy (Leiden Observatory), Michiel Min (Anton Pannekoek Instituut)

Exoplanet Theory

Development of planet formation theory by comparison with observational data

Masahiro Ogihara (NAOJ), Yasunori Hori (ABC), Takeru Suzuki (University of Tokyo), Eiichiro Kokubo (NAOJ), Alessandro Morbidelli (OCA)

Theoretical modeling of Hα spectral profile with 1D-radiation-hydrodynamic simulation: constraining the accretion rate and mass of the protoplanets PDS70b and c

Yuhiko Aoyama (Tsinghua University), Masahiro Ikoma (University of Tokyo)

Formation of Planetary Systems in Mean Motion Resonances

Su Wand (Purple Mountain Observatory), Jianghui Ji (Purple Mountain Observatory)

Directly-imaged atmospheric characterisation with TauREx retrievals

Niall Whiteford (University of Edinburgh), A. Glasse (UKATC), B. Biller (UoE), K. Rice (UoE), P. Palmer (UoE)

Disk Imaging

Observing planet formation in protoplanetary disks

Ruobing Dong (University of Victoria)

Using Debris Disks to Trace Planetary System Formation and Evolution

Meredith Ann MacGregor (Carnegie Institution for Science)

Dust production in young debris disks

Johan Olofsson (Carnegie Institution for Science), SPHERE consortium, Max Planck Tandem Group, Nucleo Milenio for Planet Formation

Optical and near-infrared scattered light imaging of protoplanetary disks

71 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Christian Ginski (Anton Pannekoek Institute for Astronomy, Amsterdam), SPHERE GTO team, DESTINYS team

The Eroding Disk of AU Mic: Implications for the Habitability of M-star Terrestrial Planets

Carol Anne Grady (Eureka Scientific), J.P. Wisniewski (U.Oklahoma), G. Schneider (U. Arizona), A. Boccaletti (LESIA), A. Gaspar (U. Arizona), J.H. Debes (STSCI), D.C. Hines (STSCI), C.C. Stark (STScI), C. Thalmann (ETH Zurich), A.-M. Lagrange (IPAG), J.-C. Augereau (IPAG), E. Sezestre (IPAG), J. Milli (ESO- Chile), T. Henning (MPIA), M.J. Kuchner (NASA)

Dust Filtration in T Tauri Star HP Cha

Mihiko Konishi (Oita University), Jun Hashimoto (ABC), Hauyu Baobab Liu (ASIAA), Ruobing Dong (University of Victoria), Matthias Samland (MPIA), Christian Ginski (University of Amsterdam), Yasuhiro Hasegawa (JPL), Takayuki Muto (Kogakuin University)

The scattering phase function of debris disks

Julien Milli (ESO), Jean-Charles Augereau (IPAG,France), Francois Menard (IPAG, France), Anny- Chantal Levasseur-Rigourd (LATMOS, France), Ryo Tazaki (Tohoku University, Japan), Johan Olofsson (Valparaiso University, Chile), Mickael Bonnefoy (IPAG, France), Christophe Pinte (Monash University, Australia)

Analysis of the population of debris disks viewed with HST

Elodie Choquet (Laboratoire d'Astrophysique de Marseille), Bin Ren (STScI), John Debes (STScI), Christopher Stark (STScI), Christine Chen (STScI), Max Millar-Blanchaer (JPL), Geoffrey Bryden (JPL), Farisa Morales (JPL), Marshall Perrin (STScI), Remi Soummer (STScI), Laurent Pueyo (STScI), Brendan Hagan (STScI), Glenn Schneider (STScI), Dean Hines (STScI), David Golimowski (STScI), Abijith Rajan (STScI)

A high-contrast SmallSat Mission Concept

Ewan S Douglas (University of Arizona), Dae Wook Kim (University of Arizona), Kate Su (University of Arizona), and the CDEEP team

A Deep Polarimetric Study of the Asymmetrical Debris Disk HD 106906

Katie Ann Crotts (University of Victoria), Brenda Matthews (National Research Council Canada), Gaspard Duchene (UC Berkeley), Paul Kalas (UC Berkeley), Tom Esposito (UC Berkeley), Max Millar-Blanchaer (JPL), Johan Mazoyer (JPL)

HD 146897; An Icy Debris Disk as seen by the Gemini Planet Imager

Schuyler Grace Wolff (Leiden Observatory), Charles Poteet (STScI), Bin Ren (JHU), Gaspard Duchene (UCB), Pauline Arriaga (UCLA), Christine Chen (STScI), Thomas Esposito (UCB), Mike Fitzgerald (UCLA), Dean Hines (STScI), Sasha Hinkley (Univ. of Exeter), Justin Hom (Arizona State Univ.), Meredith Hughes (Wesleyan Univ.), Paul Kalas (UCB), Brenda Matthews (NRC), Johan Mazoyer (JPL), Stanimir Metchev (Univ. of Western Ontario), Max Millar-Blanchaer (JPL),

72 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Jennifer Patience (Arizona State Univ.), Marshall Perrin (STScI), Abhijith Rajan (STScI), Fredrik Rantakyro (Gemini Observatory), Glenn Schneider (Univ. of Arizona), Remi Soummer (STScI), Christopher Stark (STScI), Kimberly Ward-Duong (Amherst College), Alycia Weinberger (DTM), and David Wilner (CfA).

Investigating the gas-to-dust ratio in the protoplanetary disk of HD 142527

Munetake Momose (Ibaraki University), Kang-Lou SOON (Ibaraki University), Takayuki MUTO(Kogakuin University), Takashi TSUKAGOSHI (NAOJ), Akimasa KATAOKA(NAOJ), Tomoyuki HANAWA(Chiba University), Misato FUKAGAWA(NAOJ), Kazuya SAIGO(NAOJ) and Hiroshi SHIBAI(Osaka University)

Water ice mapping toward protoplanetary disk

Mitsuhiko Honda (Okayama University of Science), Koji Murakawa (Osaka Sangyo University), Hiroshi Terada (NAOJ), Tomoyuki Kudo (NAOJ), Jun Hashimoto (ABC), Motohide Tamura (University of Tokyo, ABC), Makoto Watanabe (Okayama University of Science)

The derivation of the dust properties using the synthetic ALMA multiband analysis

Seongjoong Kim (Tokyo Institute of Technology), Hideko Nomura (NAOJ), Takashi Tsukagoshi (NAOJ), Ryogei kawabe (NAOJ), Takayuki Muto (Kogakuin University)

The detection of a dust ring beyond the outer edge of the dust disk around CR Cha

Seongjoong Kim (Tokyo Institute of Technology), Sanemichi Takahashi, Hideko Nomura, Takashi Tsukagoshi, Seokho Lee, Akimasa Kataoka (NAOJ), Takayuki Muto (Kogakuin University), Ruobing Dong (University of Victoria), Yasuhiro Hasegawa (California Institute of Technology), Jun Hashimoto, Mihoko Konishi (Astrobiology Center), Kazuhiro Kanagawa (University of Tokyo), Hauyu Baobab Liu (ASIAA), Munetake Momose (Ibaraki University), Micheal Sitko (University of Cincinnati), Kengo Tomida (Osaka University)

First detection of a very sharp ring in near-infrared light with VLT/SPHERE around HD 121617

Clement Perrot (Universidad de Valparaiso, NPF, LESIA), Olofsson Johan (Universidad de Valparaiso, NPF), Bayo Amelia (Universidad de Valparaiso, NPF), Iglesias Daniela (Universidad de Valparaiso, NPF), Montesinos Matias (Universidad de Valparaiso, NPF), Mauco Karina (Universidad de Valparaiso, NPF), Godoy Nicolas (Universidad de Valparaiso, NPF), van Holstein Rob (ESO), Kennedy Grant (University of Warwick) and Pinte Christophe (MoCA)

First resolved observations of a highly asymmetric debris disc around HD 160305 with VLT/SPHERE

Clement Perrot (Universidad de Valparaiso, NPF, LESIA), Thebault Philippe (LESIA), Lagrange Anne-Marie (IPAG), Boccaletti Anthony (LESIA), Vigan Arthur (LAM), Olofsson Johan (Universidad de Valparaiso, NPF), Bayo Amelia (Universidad de Valparaiso, NPF), Iglesias Daniela (Universidad de Valparaiso, NPF), Desidera Silvano (INAF), Augereau Jean-Charles (IPAG), Bonnefoy Mickael (IPAG), Choquet Elodie (LAM), Kral Quentin (LESIA), Loh Alan (LESIA), Maire Anne-Lise (STAR), Menard Francois (IPAG), Messina Sergio (INAF), Gratton Raffaele (INAF), the SPHERE team.

73 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

The illusive disk around TWA 7

Amelia Bayo (IFA/NPF), J. Olofsson, L. Matra, J. C. Beamin, J. Gallardo, I. de Gregorio-Monsalvo, M. Booth, C. Zamora, D. Iglesias, Th. Henning, M. R. Schreiber, and C. Caceres

The Surprising Scattering Phase Function of HR 4796 A

Johan Mazoyer (Jet Propulsion Laboratory, California Institute of Technology), Christine Chen (STScI, Baltimore, MD), Charles Poteet (STScI, Baltimore, MD), Gaspard Duchene (UC Berkeley CA), Pauline Arriaga (UCLA, CA), Max Millar-Blanchaer (JPL, Pasadena, CA) & the GPI LLP collaboration

ALMA reveals a misaligned, HCO+-rich, inner gas disk inside the large cavity of the transitional disk around J160421.7-213028

Satoshi Mayama (SOKENDAI), Eiji Akiyama(Hokkaido University), Olja Pani'c(University of Leeds), James Miley(University of Leeds), Takashi Tsukagoshi(NAOJ), Takayuki Muto(Kogakuin University), Ruobing Dong(University of Victoria), Jerome de Leon(The University of Tokyo), Toshiyuki Mizuki(JAXA), Daehyeon Oh(NMSC), Jun Hashimoto(ABC), Jinshi Sai(The University of Tokyo), Thayne Currie(Subaru Telescope), Michihiro Takami(ASIAA), Carol A. Grady(NASA), Masahiko Hayashi(JSPS), Motohide Tamura(The University of Tokyo), Shu-ichiro Inutsuka(Nagoya University)

The Hunt for Observable Signatures of Terrestrial planetary Systems (HOSTS): How Much Dust should We Expect in the Habitable Zone?

Carol Anne Grady (Eureka Scientific), J.P. Wisniewski (U.Oklahoma), G. Schneider (U. Arizona), A. Boccaletti (LESIA), A. Gaspar (U. Arizona), J.H. Debes (STSCI), D.C. Hines (STSCI), C.C. Stark (STScI), C. Thalmann (ETH Zurich), A.-M. Lagrange (IPAG), J.-C. Augereau (IPAG), E. Sezestre (IPAG), J. Milli (ESO- Chile), T. Henning (MPIA), M.J. Kuchner (NASA)

The Hunt for Observable Signatures of Terrestrial planetary Systems (HOSTS): How Much Dust should We Expect in the Habitable Zone?

Phil Hinz (University of California Santa Cruz), the HOSTS team

Debris disks imaged with the Gemini Planet Imager Exoplanet Survey

Paul Kalas (University of California Berkeley), Thomas M. Esposito, Michael P. Fitzgerald, Maxwell A. Millar-Blanchaer, Christine Chen, Marshall D. Perrin, Schuyler Wolff, Brenda Matthews, Gaspard Duchene, Katherine Follette, Stan Metchev, Pauline Arriaga, Justin Hom, Sebastian Bruzzone, and the Gemini Planet Imager Exoplanet Survey team

A Survey for Resolved Debris Disks in the Sco-Cen Association

Jennifer Patience (ASU, School of Earth and Space Exploration), Justin Hom (Arizona State University), Marshall Perrin (STScI), Tom Esposito (UC Berkeley), Johan Mazoyer (STScI), Paul Kalas (UC Berkeley), Gaspard Duchene (UC Berkeley), Elisabeth Matthews (MIT), Pauline Arriaga

74 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

(UCLA), Christine Chen (STScI), Max Millar-Blanchaer (JPL), Stan Metchev (Western Ontario), Brenda Matthews (NRC), Mike Fitzgerald (UCLA), Schuyler Wolff (Leiden)

Discovery of an azimuthal density gradient in a gas-rich debris disk possibly related to a massive collision

Garima Singh (Observatory of Paris), Ryan Boukrouche (AOPP, Physics Department, University of Oxford, UK), Anthony Boccaletti (LESIA, Observatoire de Paris, France), Trisha Bhowmik (LESIA, Observatoire de Paris, France), Clement Perrot (Instituto de Fisica y Astronomia, U. de Valparaiso, Chile), Quentin Kral (LESIA, Observatoire de Paris, France), Julien Milli (European Southern Observatory, Santaigo), Johan Olofsson (Instituto de Fisica y Astronomia, U. de Valparaiso, Chile), Johan Mazoyer (Jet Propulsion Laboratory, Pasadena, USA), the SPHERE consortium

Comparison of PSF Subtraction Algorithms on Disk Imaging Data

Justin Hom (Arizona State University), Jennifer Patience (ASU), Gaspard Duchene (UCB), Tom Esposito (UCB), Bin Ren (Caltech), Maxwell Millar-Blanchaer (JPL), Jason Wang (Caltech), Bruce MacIntosh (Stanford University), James Graham (UCB), Marshall Perrin (StScI)

Structure of the protoplanetary disk around V1094 Sco obtained from dust continuum emission and SED

Sanemichi Z. Takahashi (NAOJ), Takayuki Muto(Kogakuin University), Takashi Tsukagoshi (NAOJ), Jun Hashimoto (NAOJ)

Subaru Telescope High-contrast Observations of disks in multiple systems

Yi Yang (NAOJ), HiCIAO/AO188/SEEDS Team

New constraints on the dust and gas distribution in the LkCa 15 disk

Jin Sheng (Purple Mountain Observatory), Andrea Isella(Rice University), Pinghui Huang(PMO), Shengtai Li(LANL), Hui Li(LANL), Jianghui Ji(PMO)

SPHERE Observations of Debris Disks

Natalia Engler (ETH Zurich Institut for Particle Physics and Astrophysics)

SPHERE reveals warped disk around HD 139614

G. A. Muro-Arena (University of Amsterdam), M. Benisty, C. Ginski, C. Dominik, et al.

Disk Theory

Radiative scale-height and shadows in protoplanetary disks

75 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Matias Montesinos (Universidad de Valparaiso), Nicolas Cuello (PUC), Jorge Cuadra (PUC), Johan Olofsson (UV), Amelia Bayo (UV), Gesa H.-M. Bertrang (MPIA), Gregory J. Herczeg (KIAA), Clement Perrot (UV)

Formation of axisymmetric substructures via secular instabilities triggered by dust-gas friction and turbulent viscosity in protoplanetary disks

Ryosuke T. Tominaga (Nagoya University), Sanemichi Z. Takahashi (NAOJ), and Shu-ichiro Inutsuka (Nagoya University)

Clustering and collision statistics of dust particles in weakly compressible turbulence in protoplanetary disks

Yoshiki Sakurai (Nagoya University), Takashi Ishihara (Okayama University), Hitomi Furuya (University of Tsukuba), Masayuki Umemura (University of Tsukuba), and Kenji Shiraishi (Nagoya University)

Radiation Hydrodynamics Simulations of Photoevaporating Protoplanetary Disks with Various Metallicities

Riouhei Nakatani (RIKEN), Takashi Hosokawa (Kyoto University), Naoki Yoshida (The University of Tokyo), Hideko Nomura (NAOJ), and Rolf Kuiper (University of Tubingen)

Effect of dust size and structure on scattered-light images of protoplanetary disks

Ryo Tazaki (Tohoku University), Hidekazu Tanaka (Tohoku University), Takayuki Muto (Kogakuin University), Akimasa Kataoka (NAOJ), Satoshi Okuzumi (Tokyo Institute of Technology)

Dispersal of Protoplanetary Disks with Magnetically-driven and Photoevaporative Winds

Masanobu Kunimoto (Kurume University), Takeru K. Suzuki (University of Tokyo), and Shu-ichiro Inutsuka (Nagoya University)

Instrument and Technology

Overview and on-sky results of the vector-Apodizing Phase Plate coronagraph

David Doelman (Leiden Observatory), Steven Bos (Leiden Observatory), Emiel Por (Leiden Observatory), Alex Bohn (Leiden Observatory), Jos de Boer (Leiden Observatory), Kelsey Miller (Leiden Observatory), Gilles Otten (LAM), Matthew Kenworty (Leiden Observatory), Christoph Keller (Leiden Observatory), Frans Snik (Leiden Observatory), SCExAO team, CHARIS team, LMIRCam team, ALES team, MagAO team, MagAO-X team, HiCIBaS team, ERIS team, METIS team, MICADO team.

Focal-plane wavefront sensing with the vAPP: on-sky demonstration at SCExAO

76 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Steven Peter Bos (Leiden Observatory), David Doelman (Leiden Observatory), Julien Lozi (NAOJ), Olivier Guyon (NAOJ, University of Arizona, ABC), Christoph Keller (Leiden Observatory), Kelsey Miller (Leiden Observatory), Nemanja Jovanovic (CalTech), Frantz Martinache (Observatoire de la Cote dAzur), Frans Snik (Leiden Observatory)

Polarization-dependent beam shifts upon metallic reflection in diffraction-limited astronomical telescopes and instruments

Rob van Holstein (Leiden Observatory), Christoph Keller (Leiden Observatory), Frans Snik (Leiden Observatory), Steven Bos (Leiden Observatory), Julien Milli (European Southern Observatory), Hans Martin Schmid (ETH Zurich), Jozua de Boer (Leiden Observatory)

The Decadal Survey Testbed: Demonstrating Technology for Imaging Earth-like Exoplanets with Future Space Telescopes

Garreth Ruane (Jet Propulsion Laboratory), Keith Patterson, Byoung-Joon Seo, Camilo Mejia Prada, Nick Siegler, Brendan Crill

Bringing high-spectral resolution to VLT/SPHERE with a coupling to VLT/CRIRES+: status of the HiRISE project

Arthur Vigan (Laboratoire d'Astrophysique de Marseille / CNRS), Gilles Otten (Laboratoire d'Astrophysique de Marseille) Eduard Muslimov (Laboratoire d'Astrophysique de Marseille) Yannick Charles (Laboratoire d'Astrophysique de Marseille) Raphael Pourcelot (Laboratoire d'Astrophysique de Marseille) Ulf Seemann (University of Gottingen) Kjetil Dohlen (Laboratoire d'Astrophysique de Marseille) Mathis Houlle (Laboratoire d'Astrophysique de Marseille) Elodie Choquet (Laboratoire d'Astrophysique de Marseille) HiRISE team

On-sky validation of the ZELDA wavefront sensor for the calibration of non-common path aberrations in VLT/SPHERE

Arthur Vigan (Laboratoire d'Astrophysique de Marseille / CNRS), Mamadou N'Diaye (Laboratoire Lagrange) Kjetil Dohlen (Laboratoire d'Astrophysique de Marseille) Jean-Francois Sauvage (Laboratoire d'Astrophysique de Marseille / ONERA) Julien Milli (ESO) Gerard Zins (ESO) Cyril Petit (ONERA) Zahed Wahhaj (ESO) Faustine Cantalloube (MPIA) ZELDA team

Mach-Zehnder Wavefront sensor for XAO: From laboratory tests to on sky measurements using the SCAO capability of CANARY at the William Hershel Telescope

Maud Langlois (CNRS/CRAL), M. Loupias (CNRS/CRAL), N. Dubost (CfAI),, N. Bharmal (CfAI), , C. Schott (CRAL), M. Tallon (CRAL), E. Thiebaut (CRAL), L. Bardou (CfAI), T. Buey(LESIA) , F. Chemla (GEPI), M. Cohen (GEPI), E. Gendron (LESIA), T. Morris(CfAI), J. Osborn (CfAI),L. Staykov (CfAI)

Partially Filled Aperture Interferometric Telescopes Achieving Large Aperture and Coronagraphic Performance — The Exo-Life Finder (ELF) Telescope

Gil Moretto (Centre de Recherche Astrophysique de Lyon-CRAL/CNRS), Jeff Kuhn (IfA, University of Hawaii, USA), Jean-Fabien Capsal (LGEF/INSA-Lyon, FRANCE), David Audigier (LGEF/INSA-Lyon, FRANCE), Kritsadi Thetpraphi (LGEF/INSA-Lyon, FRANCE), Maud Langlois

77 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

(CRAL/CNRS, Saint-Genis Laval, FRANCE ), Michel Tallon (CRAL/CNRS, Saint-Genis Laval, FRANCE) and Svetlana Berdugyna (KIS, Universitat Freiburg, GERMANY)

Spatial Linear Dark Field Control on SCExAO

Kelsey Lynn Miller (Leiden Observatory, Leiden University), Olivier Guyon (National Institutes of Natural Sciences, Subaru Telescope, National Observatory of Japan) Julien Lozi (National Institutes of Natural Sciences, Subaru Telescope, National Observatory of Japan) Steven Bos (Leiden Observatory, Leiden University) David Doelman (Leiden Observatory, Leiden University) Jared Males (University of Arizona, Steward Observatory) Frans Snik (Leiden Observatory, Leiden University)

Heritage of technology for mid-infrared coronagraph onboard space-borne telescopes for exoplanet characterization

Keigo Enya (JAXA/ISAS), Takayuki Kotani (ABC) Aoi Takahashi (ABC) Kanae Haze (JAXA) Lyu Abe (Observatoire de la Cote d'Azur/UNS)

Speckle Subtraction: Limitations and the Path Forward

Benjamin L. Gerard (University of Victoria), Christian Marois (NRC HAA), Raphael Galicher (Observatoire de Paris), Jean-Pierre Veran (NRC HAA), Thayne Currie (NASA Ames)

Active Speckle Control with Microwave Kinetic Inductance Detectors

Neelay Hitesh Fruitwala (University of California at Santa Barbara), Alex B. Walter (University of California at S anta Barbara), Olivier Guyon (National Astronomical Observatory of Japan), Julien Lozi (National Astronomical Observatory of Japan), Benjamin A. Mazin (University of California at Santa Barbara)

New Symmetrical Formulation of Hexagonally Segmented Telescopes

Satoshi Itoh (Osaka University), Taro Matsuo (Osaka University), Hiroshi Shibai (Osaka University), Takahiro Sumi (Osaka University)

Laboratory demonstration of 1e-10 contrast with a sub-scale starshade external occulter

Anthony Harness (Princeton University), N. Jeremy Kasdin (Princeton), Stuart Shaklan (JPL), Michael Galvin (Princeton), Phil Willems (JPL), Kunjithapatham Balasubramanian (JPL), Victor White (JPL), Karl Yee (JPL), Richard Muller (JPL), Philip Dumont (JPL), Simon Vuong (JPL)

Upgrading the Gemini planet imager: GPI 2.0

Jeffrey K Chilcote (University of Notre Dame), Quinn Konopacky (UCSD), Bruce Macintosh (Stanford), Dmitry Savransky (Cornell), Rob De Rosa (Stanford), Christian Marois (HAA), Marshall Perrin (STScI)

Status of the Phase II design and development of the Keck Planet Imager and Characterizer

78 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Jacklyn Pezzato (California Institute of Technology), Nemanja Jovanovic (Caltech), Garreth Ruane (JPL), Jason Wang (Caltech), James K. Wallace (JPL), Jennah Colborn (Caltech), Randall D. Bartos (JPL), Jacques-Robert Delorme (Caltech), Dimitri Mawet (Caltech), Charlotte Z. Bond (WMKO), Sylvain Cetre (WMKO), Daniel Echeverri (Caltech), Rebecca Jensen-Clem (UC Berkeley), Scott Lilley (WMKO), Peter Wizinowich (WMKO), Ed Wetherell (WMKO)

NASA’s S5 Starshade Technology Development Activity

Phil Willems (NASA Jet Propulsion Laboratory), S5 Team,

Combination of apodized pupil and phase mask coronagraph for Subaru Telescope

Jun Nishikawa (NAOJ/SOKENDAI/ABC), Naoshi Murakami (Hokkaido Univ.), Keiichiro Habu (Hokkaido Univ.), Hikaru Ichien (Hokkaido Univ.), Julien Lozi (Subaru Telescope), Olivier Guyon (Subaru Telescope), Kosuke Kumaki (Nihon Univ.), Shiomi Kumagai (Nihon Univ.)

Pushing the Limits of Exoplanet Discovery via Direct Imaging with Deep Learning

Kai Hou Yip (UCL), Nikolaos Nikolaou(UCL), Piero Coronica(Research Software Engineering, University of Cambridge), Angelos Tsiaras(UCL), Billy Edwards(UCL), Quentin Changeat(UCL), Mario Morvan(UCL), Beth Biller(ROE,University of Edinburgh), Sasha Hinkley(University of Exeter), Jeffrey Salmond(Research Software Engineering, University of Cambridge), Matthew Archer(Research Software Engineering, University of Cambridge), Paul Sumption(Research Software Engineering, University of Cambridge), Elodie Choquet(Aix Marseille Univ), Remi Soummer(STScI), Laurent Pueyo(STScI), Ingo P. Waldmann(UCL)

Comparing Focal Plane Wavefront Sensors on THD2 bench : Self-coherent camera, Pair Wise Probing and COFFEE

Axel Potier (LESIA - Observatoire de Paris), Pierre Baudoz (LESIA), Raphael Galicher (LESIA), Laurent Mugnier (ONERA), Olivier Herscovici-Schiller (ONERA) and Jean-Francois Sauvage (ONERA, LAM)

Performance simulations of the high-res characterization of directly imaged planets with HiRISE

Gilles Otten (Laboratoire d'Astrophysique de Marseille), HiRISE team: Arthur Vigan (PI), Eduard Muslimov, Yannick Charles, Kjetil Dohlen, Raphael Pourcelot, Jean-Luc Beuzit, Matthis Houlle, Elodie Choquet, Nicolas Tchoubaklian, Jean-Francois Sauvage, Paul Cristofari, Pierre Tomlinson (Laboratoire d'Astrophysique de Marseille), Ulf Seemann, Ansgar Reiners (University of Gottingen), Markus Kasper, Reinhold Dorn, Julien Milli, Gerard Zins, Pedro Figueira (ESO), Mark Phillips, Isabelle Baraffe (University of Exeter), David Mouillet, Alexis Carlotti (IPAG), Mamadou N'Diaye, Remi Flamary, David Mary (Laboratoire Lagrange), Anthony Boccaletti, Benjamin Charnay (LESIA)

Sensitivity to telescope aberrations for exoplanet detection with the LUVOIR coronagraph instrument ECLIPS

Roser Juanola-Parramon (NASA Goddard Space Flight Center), Neil Zimmerman (NASA GSFC), Tyler Groff (NASA GSFC), Laurent Pueyo (STScI)

79 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Imaging and Characterization of Rocky Earth-size Habitable Zone Planets in the Solar Neighborhood with TMT

Christian Marois (National Research Council of Canada), William Thompson (University of Victoria), Kathryn Jackson (National Research Council of Canada)

New NIR Polarimetric Differential Imaging Modes on the Subaru Coronagraphic Extreme Adaptive Optics Instrument

Jin Zhang (The University of Tokyo), Motohide Tamura (The University of Tokyo, ABC, NAOJ), Olivier Guyon (The University of Arizona, ABC, NAOJ), Tomoyuki Kudo (NAOJ), Julien Lozi (NAOJ), Barnaby Norris (The University of Sydney), Nemanja Jovanovic (California Institute of Technology), Tyler Groff (NASA GSFC), Jeff Chilcote (University of Notre Dame), Jeremy Kasdin (Princeton University), Steven Bos (Leiden University), Frans Snik (Leiden University), David Doelman (Leiden University), Frantz Martinache (Observatoire de la Cote d'Azur)

Results with FALCO, a Software Package for Coronagraphic Wavefront Correction

A J Eldorado Riggs (Jet Propulsion Laboratory), Garreth Ruane (JPL), Erkin Sidick (JPL), Carl Coker (JPL), Navtej Saini (JPL), Jorge Llop-Sayson (Caltech)

Vortex Fiber Nulling for Exoplanet Observations: Concept, Laboratory Results, and Planned On- Sky Deployment

Daniel Echeverri (Caltech), Garreth Ruane (JPL), Nemanja Jovanovic (Caltech), Thomas Hayama (Caltech), Jacques-Robert Delorme (Caltech), Charlotte Bond (IfA), Jacklyn Pezzato (Caltech), Dimitri Mawet (JPL/Caltech), J. Kent Wallace (JPL).

Development of the Extremely High-Contrast, High Spectral Resolution Spectrometer REACH for the Subaru Telescope

Takayuki Kotani (Astrobiology center/NAOJ), Hajime Kawahara (University of Tokyo), Masato Ishizuka (University of Tokyo), Nemanja Jovanovic (Caltech Optical Observatories), Olivier Guyon (Subaru), Julien Lozi (Subaru), Sebastien Vievard (Subaru), Ananya Sahoo (Subaru), Motohide Tamura (University of Tokyo)

Wavefront control and calibration for the WFIRST Coronagraph Instrument

Eric Cady (Jet Propulsion Laboratory, California Institute of Technology), WFIRST CGI instrument team

Results from Microwave Kinetic Inductance Detectors for Exoplanet Direct Imaging

Ben Mazin (University of California Santa Barbara), Jeb Bailey (University of California Santa Barbara) Clint Bockstiegel (University of California Santa Barbara) Michal Bottom (U. Hawaii) Timothy Brandt (University of California Santa Barbara) Bruce Bumble (NASA Jet Propulsion Lab) Gregoire Coiffard (University of California Santa Barbara) Kristina Davis (University of California Santa Barbara) Rupert Dodkins (University of California Santa Barbara) Neelay Fruitwala (University of California Santa Barbara) Olivier Guyon (Subaru/Arizona) Nemanja Jovanovic (Caltech Optical Observatories) Isabel Lipartito (University of California Santa Barbara) Julien Lozi

80 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

(Subaru Telescope) Dimitri Mawet (California Institute of Technology) Seth Meeker (NASA Jet Propulsion Lab) Jenny Smith (University of California Santa Barbara) Sarah Steiger (University of California Santa Barbara) Noah Swimmer (University of California Santa Barbara) Alex Walter (University of California Santa Barbara) Nick Zobrist (University of California Santa Barbara)

Theoretical Performance Limits for Coronagraphs on Obstructed and Unobstructed Apertures: How Much Can Current Designs be Improved?

Ruslan Belikov (NASA Ames Research Center), Jeff Jewell (NASA JPL) Dan Sirbu (NASA ARC) Eduardo Bendek (NASA JPL) Stuart Shaklan (NASA JPL) Olivier Guyon (NAOJ / Subaru Telescope) Christopher Stark (STScI)

Applications of Multi-Star Wavefront Control to WFIRST, HABEX, and LUVOIR

Dan Sirbu (NASA Ames Research Center / BAERI), Ruslan Belikov (NASA Ames), Eduardo Bendek (JPL/Caltech), Chris Henze (NASA Ames), Eugene Pluzhnyk (NASA Ames/BAERI)

Detecting companions inside the coronagraphic regime with nulling interferometry

Eugene Serabyn (Jet Propulsion Laboratory, California Institute of Technology), B. Mennesson (JPL), S. R. Martin (JPL), K. Liewer (JPL), J. Kuhn (Univ. Bern)

Spectroscopy below the diffraction limit with FIRSTv2 at the Subaru Telescope

Elsa Huby (LESIA, Observatoire de Paris), Sebastien Vievard (NAOJ), Nick Cvetojevic (Observatoire de la Cote d'Azur), Sylvestre Lacour (Observatoire de Paris), Guillermo Martin (Institut de Planetologie et d'Astrophysique de Grenoble), Olivier Guyon (NAOJ), Julien Lozi (NAOJ), Nemanja Jovanovic (Caltech), Guy Perrin (Observatoire de Paris), Franck Marchis (SETI), Gaspard Duchene (UC Berkeley), Takayuki Kotani (NAOJ) and Vincent Lapeyrere (Observatoire de Paris)

New high contrast technology demonstrations at the High-Contrast Spectroscopy Testbed for Segmented Telescopes (HCST)

Jorge Llop Sayson (California Institute of Technology (Caltech)), Garreth Ruane (JPL), Carl Cocker (JPL), Dimitri Mawet (Caltech), Nemanja Jovanovic (Caltech)

Assembly, Integration, and Testing of the Deformable Mirror Demonstration Mission (DeMi) CubeSat Payload

Rachel Elizabeth Morgan (MIT Department of Aeronautics and Astronautics), Gregory Allan (MIT); Ewan Douglas (MIT); Paula do Vale Pereira (MIT); Mark Egan (MIT); Gabor Furesz (MIT); Jennifer Gubner (MIT); Christian Haughwout (MIT); Bobby Holden (MIT); John Merk (Aurora Flight Sciences); Thomas Murphy (MIT); Abigail Stein (MIT); Yinzi Xin (MIT); Kerri Cahoy (MIT)

Robust high contrast imaging with kernel-nulling interferometry

Frantz Martinache (Universite Cote d'Azur, Observatoire de la Cote d'Azur, CNRS, Laboratoire Lagrange, France), Nick Cvetojevic (Universite Cote d'Azur, Observatoire de la Cote d'Azur, CNRS, Laboratoire Lagrange, France)

81 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Imaging short orbit exoplanets from the ground with novel Apodized Pupil Lyot Coronagraphs

Mamadou N'Diaye (Observatoire de la Cote d'Azur), Alexis Carlotti (IPAG)

Progress Towards a Laboratory Demonstration of a Multi-Object, Single-Mode Fiber Spectrograph

Carl Coker (Jet Propulsion Laboratory), Stuart Shaklan (JPL), Jorge Llop Sayson (Caltech), Nemanja Jovanovic (Caltech), Dimitri Mawet (Caltech), A J Eldorado Riggs (JPL), Garreth Ruane (JPL)

SCExAO: Current status and upgrades

Julien Lozi (NAOJ - Subaru Telescope), Olivier Guyon (Subaru Telescope, ABC, University of Arizona), Sebastien Vievard (Subaru Telescope), A. Sahoo (Subaru Telescope), N. Jovanovic (CalTech), B. Norris (University of Sydney), B. Mazin (UCSB), A. Walter (UCSB), P. Tuthill (University of Sydney), T. Kudo (Subaru Telescope), H. Kawahara (University of Tokyo), T. Kotani (NAOJ), M. Ishizuka (University of Tokyo), M. Ireland (ANU), N. Cvetojevic (Observatoire de la Cote d'Azur), E. Huby (LESIA), S. Lacour (LESIA), T. D. Groff (NASA Goddard), J. Chilcote (University of Notre-Dame), J. Kasdin (Princeton), F. Martinache (Observatoire de la Cote d'Azur), R. Laugier (Observatoire de la Cote d'Azur), J. Knight (University of Arizona), S. Bos (Leiden Observatory), F. Snik (Leiden Observatory), D. Doelman (Leiden Observatory), E. Bendek (JPL), R. Belikov (NASA Ames), T. Currie (NASA Ames), Y. Minowa (Subaru Telescope), C. Clergeon (Subaru Telescope), N. Takato (Subaru Telescope), M. Tamura (ABC, University of Tokyo), J. Zhang (University of Tokyo), H. Takami (NAOJ), M. Hayashi (NAOJ)

Polychromatic analysis of the coronagraphs in SCExAO

Julien Lozi (NAOJ - Subaru Telescope), O. Guyon (Subaru Telescope, ABC, University of Arizona), N. Jovanovic (CalTech), S. Vievard (Subaru Telescope), A. Sahoo (Subaru Telescope), F. Martinache (Observatoire de la Cote d'Azur), J. Kuhn (ETH), E. Serabyn (JPL), N. Murakami (Hokkaido University), J. Nishikawa (Subaru Telescope), F. Snik (Leiden Observatory), D. Doelman (Leiden Observatory), S. Bos (Leiden Observatory), T. Kudo (Subaru Telescope), T. D. Groff (NASA Goddard), J. Chilcote (University of Notre-Dame), J. Kasdin (Princeton), M. Tamura (ABC, University of Tokyo), T. Currie (NASA Ames)

Overview of the THD2 performance

Pierre Baudoz (Observatoire de Paris), Raphael Galicher (Obs. Paris) and the THD2 Team

SLM-based Digital Adaptive Coronagraphy: Status, performance update, and future prospects

Jonas G Kuhn (Center for Space and Habitability (CSH), University of Bern), Polychronis Patapis (ETH Zurich)

XAO-assisted coronagraphy with SHARK-NIR: from simulations to laboratory tests

Elena Carolo (INAF - OAPd), Umbriaco G. (INAF OAPd, UniPD), Vassallo D. (INAF OAPd), Farinato J. (INAF OAPd), Agapito G. (INAF OAA), Baudoz P. (LESIA), Bergomi M. (INAF

82 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

OAPd), Biondi F. (INAF OAPd), Carlotti A. (IPAG), Chinellato S. (INAF OAPd), De Pascale M. (INAF OAPd), D Orazi V. (INAF OAPd), Esposito S. (INAF OAA), Greggio D. (INAF OAPd), Magrin D. (INAF OAPd), Marafatto L. (INAF OAPd), Mesa D. (INAF OAPd), Pinna E. (INAF OAA), Puglisi A. (INAF OAA), Stangalini M. (INAF OAR) and Viotto V. (INAF OAPd)

Overview of focal plane wavefront sensors to correct for the Low Wind Effect on SUBARU/SCExAO

Sebastien B Vievard (ABC, LESIA, Subaru Telescope), Aurelie Bonnefois (ONERA), Steven Bos (Leiden University), Frederic Cassaing (ONERA), Olivier Guyon (ABC, Subaru Telescope, University of Arizona, NASA-JPL), Nemanja Jovanovic (Caltech), Christoph Keller (Leiden University), Julien Lozi (Subaru Telescope), Frantz MArtinache (Observatoire de la Cote d'Azur), Laurent Mugnier (ONERA), Mamadou NDiaye (Observatoire de la Cote d'Azur), Barnaby Norris (Univerity of Sydney), Jean-Francois Sauvage (ONERA), Ananya Sahoo (Subaru Telescope), Frans Snik (Leiden University), Mike Wilby (Leiden University)

Laboratory demonstration of high contrast imaging on segmented apertures: Results from STScI HiCAT testbed

Iva Laginja (Space Telescope Science Institute/ONERA), Greg Brady (STScI), Toma Comeau (STScI), Julia Fowler (STScI), Rob Gontrum (STScI), Maggie Kautz (University of Arizona), Heather Kurtz (STScI), Evelyn McChesney (STScI), James Noss (STScI), Marshall Perrin (STScI), Peter Petrone (STScI), Laurent Pueyo (STScI), Anand Sivaramakrishnan (STScI), Ana-Maria Valenzuela (STScI), Sam Weinstock (STScI), Scott Will (Rochester University/STScI), Rebecca Zhang (Caltech), Keira Brooks (STScI), Marc Ferrari (Laboratoire d'Astrophysique de Marseille), Kevin Fogarty (Caltech), John Hagopian (Advanced NanoPhotonics, Inc.), Emmanuel Hugot (Laboratoire d'Astrophysique de Marseille), Roser Juanola-Parramon (Goddard Space Flight Center), Lucie Leboulleux (Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Paris), Johan Mazoyer (JPL/Caltech), Laurent Mugnier (ONERA), Mamadou N'Diaye (Observatoire de la Cote d'Azur, Nice), Emiel Por (Leiden University), Jean-Francois Sauvage (Laboratoire d'Astrophysique de Marseille/ONERA), Nathan Scott (Johns Hopkins University), Ron Shiri (Goddard Space Flight Center), Neil Zimmerman (Goddard Space Flight Center), Remi Soummer (STScI)

Astrometry and Photometry with Satellite Speckles

Ananya Sahoo (Subaru Telescope, NAOJ), Olivier Guyon (Subaru Telescope), Julien Lozi (Subaru Telescope), Sebastien Vievard (Subaru Telescope), Jeffery Chilcote (University of Notre Dame), Nemanja Jovanovic (Caltech), Frantz Martinache (Universite Cote d'Azur), Timothy Brandt (UCSB), Tyler Groff (NASA Goddard)

The Phase-Apodized-Pupil Lyot Coronagraph (PAPLC): a simple, high-performance Lyot-style coronagraph with a small inner working angle

Emiel Por (Leiden Observatory)

Implementing Multi-wavelength Fringe Tracking for the LBTI's Phase Sensor, PHASECam

83 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Erin Maier (University of Arizona), Phil Hinz (University of California Santa Cruz) Denis Defrere (Liege Space Center, University of Liege) Paul Grenz (University of Arizona) Steve Ertel (University of Arizona) Eckhart Spalding (University of Arizona)

Prototyping High Contrast Imaging for ELTs on SCExAO: Users’ Guide and Recent Highlights

Olivier Guyon (Subaru Telescope / NAOJ, ABC & Univ. of Arizona), Theo Anagnos (Macquarie Univ.), Steven Bos (Leiden Univ.), Jeffrey Chilcote (Univ. Notre Dame), Christophe Clergeon (Subaru Telescope), Thayne Currie (NASA Ames & Subaru Telescope), Nick Cvetojevic (Univ. of Nice), David Doelman (Leiden Univ.), Rich Frazin (Univ. of Michigan), Damien Gratadour (Observatoire de Paris & Australian National Univ.), Tyler D. Groff (NASA GSFC), Derek Hand (Subaru Telescope), Elsa Huby (Observatoire de Paris), Michael Ireland (Australian National Univ.), Masato Ishizuka (Univ. of Tokyo), Nemanja Jovanovic (Caltech), Hajime Kawahara (Univ. of Tokyo), Justin Knight (Univ. of Arizona), Takayuki Kotani (ABC), Tomoyuki Kudo (Subaru Telescope), Sylvestre Lacour (Observatoire de Paris), Romain Laugier (Observatoire de Nice), Julien Lozi (Subaru Telescope), Hatem Ltaief (KAUST), Jared Males (Univ. of Arizona), Yosuke Minowa (Subaru Telescope), Marc-Antoine Martinod (Univ. of Sydney), Frantz Martinache (Univ. of Nice), Ben Mazin (UCSC), Naoshi Murakami (Hokkaido Univ.), Jun Nishikawa (NAOJ), Barnaby Norris (Univ. of Sydney), Prashant Pathak (ESO), Ananya Sahoo (Subaru Telescope), Chrisitan Schwab (Univ. of Macquarie), Eugene Serabyn (JPL), Arnaud Sevin (Observatoire de Paris), Nour Skaf (Subaru Telescope), Frans Snik (Leiden Univ.), Peter Tuthill (Univ. of Sydney), Sebastien Vievard (Subaru Telescope & ABC), Matt Wahl (Subaru Telescope), Alex Walter (UCSB), Alyson Wong (Univ. of Sydney), Jin Zhang (Univ. of Tokyo)

Overview of the coronagraphic capabilities of SHARK-NIR, the second-generation high contrast imager for the Large Binocular Telescope

Daniele Vassallo (INAF-Osservatorio Astronomico di Padova), Jacopo Farinato (INAF-OAPD), Marco Stangalini (ASI), Elena Carolo (INAF-OAPD), Alexis Carlotti (IPAG), Guido Agapito (INAF-OAA), Alfio Puglisi (INAF-OAA), Cristophe Verinaud (IPAG), Pierre Baudoz (LESIA), Valentina Viotto (INAF-OAPD), Maria Bergomi (INAF-OAPD), Davide Greggio (INAF-OAPD), Luca Marafatto (INAF-OAPD), Valentina D Orazi (INAF-OAPD) and Dino Mesa (INAF-OAPD)

Deep Neural Networks Improve the Dynamic Range of Lyot-based Low Order Wavefront Sensing

Gregory W. Allan (Massachusetts Institute of Technology), Iksung Kang (MIT) Ewan S. Douglas (MIT) Changyeob Baek (MIT) Clara Park (MIT) George Barbastathis (MIT) Kerri Cahoy (MIT)

SISTER: Simulating Exoplanetary Systems as observed with Starshade

Sergi Hildebrandt (JPL/Caltech), Stuart Shaklan (JPL)

An Introduction to SCALES, the Next-Generation Exoplanet Spectrograph

Richard Deno Stelter (UCO/UC Santa Cruz), Andrew Skemer (UCSC) Michael Fitzgerald (UCLA) Dimitri Mawet (CIT) Timothy Brandt (UCSB) Marc Kassis (W.M. Keck Observatory) Renate Kupke (UCSC) Matt Radovan (UCSC)

Towards High Throughput and Low-Order Aberration Robustness for Vortex Coronagraphs with Central Obstructions

84 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Kevin Fogarty (California Institute of Technology), Dimitri Mawet (California Institute of Technology) Johan Mazoyer (Jet Propulsion Laboratory)

The Parabolic Deformable Mirror Testbed at Goddard Space Flight Center

Tyler Groff (NASA GSFC), Hari Subedi, NASA GSFC Roser Juanola-Parramon, NASA GSFC Neil T. Zimmerman, NASA GSFC Michael W. McElwain, NASA GSFC

The Promise of Diffraction Limited Spectrometers for Exoplanet Characterization

Charles Beichman (NASA Exoplanet Science Institute/IPAC), Charles Beichman (NExScI), Rene Doyon (Univ. de Montreal), Mike Fitzgerald (UCLA), Jason Fucik (Caltech) ,Rose Gibson (Columbia College), David Hover (Caltech), Quinn Konopacky (UCSD), Nemanja Jovanovic (Caltech), Stephanie Leifer (JPL) ,Dimitri Mawet (Caltech), Rebecca Oppenheimer (AMNH), Peter Plavchan (George Mason Univ), Motohide Tamura (Univ Tokyo), Gautam Vasisht (JPL)

Developing and Demonstrating Linear Dark Field Control for Exo-Earth Imaging with the Ames Coronagraph Experiment Testbed

Thayne Currie (NASA-Ames Research Center), Eugene Pluzhnik, Ruslan Belikov, Olivier Guyon, Kelsey Miller, Jared Males

Observation/Data reduction Techniques

Exploring the limits of directly imaging exoplanets with the Medium Resolution Imaging Spectrograph on JWST MIRI

Polychronis Patapis (ETH Zurich), Adrian Glauser (ETH Zurich), Sascha Quanz (ETH Zurich)

A vector Apodising Phase Plate view of an exoplanet atmosphere

Ben Sutlieff (University of Amsterdam), Jayne Birkby (University of Amsterdam), Matthew Kenworthy (Leiden University), Katie Morzinski (University of Arizona), Jared Males (University of Arizona), Alexander Bohn (Leiden University), David Doelman (Leiden University), David Charbonneau (Harvard-Smithsonian Center for Astrophysics)

Atmospheric retrievals of directly imaged planets using TauREx3 and deep learning

Ingo Waldmann (University College London (UCL)), Ahmed Al-Refaie (UCL), Quentin Changeat (UCL)

Beyond Gaussianity for the speckle statistics, a new consensus for post-processing of high- contrast images.

Faustine Cantalloube (Max Planck Institute for Astronomy (MPIA)), Benoit Pairet (UCLouvain), Laurent Jacques (UCLouvain), Wolfgang Brandner (MPIA), Laurent Mugnier (Onera)

85 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Refining exoplanet atmospheric retrievals with information-theoretic methods

Nikolaos Nikolaou (University College London), Quentin Changeat (University College London), Hai Hou Yip (University College London), Angelos Tsiaras (University College London), Ingo Waldmann (University College London), Giovanna Tinetti (University College London)

Data Processing and Calibrations for the Gemini Planet Imager Exoplanet Survey

Marshall Perrin (Space Telescope Science Institute), Rob De Rosa (Stanford), Jeff Chilcote (University of Notre Dame), Tom Esposito (UC Berkeley), Quinn Konopacky (UC San Diego), Max Millar-Blanchaer (Caltech), Eric Nielsen (Stanford), Meiji Nguyen (UC Berkeley), JB Ruffio (Stanford), Melisa Talis (Stanford), Jason Wang (Caltech) and the GPI Exoplanet Survey Team

Studying giant planet formation with Fourier plane imaging techniques

Jens Kammerer (European Southern Observatory/ANU), Michael Ireland (ANU), Antoine Merand (ESO)

A highly-automated end-to-end pipeline to reduce VLT/SPHERE-IRDIS polarimetric data

Rob van Holstein (Leiden Observatory), Christian Ginski (University of Amsterdam), Julien Milli (European Southern Observatory), Jozua de Boer (Leiden Observatory), Frans Snik (Leiden Observatory), Julien Girard (Space Telescope Science Institute)

Numerical Investigations of Coronagraphic Self-Calibration

Yinzi Xin (MIT), Romain Laugier (Universite Cote d'Azur), Ewan Douglas (University of Arizona), Kerri Cahoy (MIT)

Reconciling kernel-phase and coronagraphy: new steps towards combining the performance of opposing techniques.

Romain Laugier (Universite Cote d'Azur), Frantz Martinache (Universite Cote d'Azur), Nick Cvetojevic (Universite Cote d'Azur), Mamadou N'Diaye (Universite Cote d'Azur), Alban Ceau (Universite Cote d'Azur), David Mary (UUniversite Cote d'Azur)

High-contrast Imaging technique combining IRS and ADI

Gang Zhao (Nanjing Institute of Astronomical Optics Technology), Jiangpei Dou (NIAOT), Deqing Ren(CSUN)

Exoplanet detection: A temporal approach for increasing contrast performance close to the inner working angle

Matthias Samland (Max Planck Institute for Astronomy), SPHERE Collaboration

New algorithms to improve the quality of NACO coronagraphic images.

86 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Nicolas Ignacio Godoy Barraza (Universidad de Valparaiso), Johan Olofsson (IFA-UV, NPF), Amelia Bayo (IFA-UV, NPF), NACO-ISPY team

Comparison between SPHERE and GPI astrometries

Anne-Marie LAGRANGE (IPAG CNRS) Jason Wang, SPHERE and GPI consortia

Combination of Direct and Indirect Techniques

Revealing exoplanet atmospheres by combining high contrast imaging with high resolution spectroscopy

Jayne Birkby (University of Amsterdam)

Results from the Beta Pictoris b Hill Sphere Transit Campaign

Matthew Kenworthy (Leiden Observatory), K. Zwintz (U. Innsbruck), T. Guillot (U. Nice), P. Kalas (Berkeley), A. Lecavelier (U. Paris), Anne-Marie Lagrange (U. Grenoble), A. Vidal Madjar (U. Grenoble), Lifan Wang (U. Bejing), Blaine Lomberg (U. Cape Town), Lyu Abe (Obs. Nice), S. Crawford (STScI), Nick Suntzeff (U. Texas), Djamel Mekarnia (Obs. Nice), S Lacour (U. Paris), Zhang Hui (U. Bejing), N. Mathias (Obs. Nice), H. Beust (Obs. Paris), K. Flavien (Obs. Paris), E. de Mooij (U. Dublin)m P. A. Wilson (U. Warwick), M. Ireland (ANU), S. N. Mellon, (U. Rochester), E. Mamajek, (JPL, U. Rochester), K. B. Stevenson (STScI), I. Laginja (STScI).

Looking for Planets in all the Right Places: Target Selection for Direct Imaging

Dmitry Savransky (Cornell University), Carlos Gascon (Universitat Politecnica de Catalunya), Nathaniel Kinzly (Cornell University)

The SPHERE view of our closest multi-planetary system: Proxima Centauri

Alice Zurlo (Universidad Diego Portales), SPHERE team

Combining high contrast imaging and radial velocities to constrain the planetary architecture of nearby stars

Anna Boehle (ETH Zurich), Sascha P. Quanz (ETH Zurich), Christophe Lovis (Observatoire Astronomique de l'Universite de Geneve), Damien Segransan (Observatoire Astronomique de l'Universite de Geneve), Stephane Udry (Observatoire Astronomique de l'Universite de Geneve), Daniel Apai (University of Arizona)

Masses, Orbits, and New Planets and Brown Dwarfs from Combining Imaging with Astrometry and Radial Velocity

87 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Timothy David Brandt (University of California, Santa Barbara), Trent Dupuy (Gemini), Brendan Bowler (UT Austin), Jackie Faherty (AMNH), G. Mirek Brandt (UCSB), Yiting Li (UCSB), Minghan Chen (UCSB), Daniella Bardalez-Gagliuffi (AMNH), Daniel Michalik (ESA), Christoph Baranec (UH)

The 2019 WFIRST Exoplanet Imaging Data Challenge

Julien H Girard (Space Telescope Science Institute (STScI)), Junellie Gonzalez-Quiles (GSFC) Sergi Hildebrandt (JPL) Stephen Kane (UCR) Davy Kirkpatrick (IPAC) Zhexing Li (UCR) Avi Mandell (GSFC) Tiffany Meshkat (IPAC) Maggie Turnbull (SETI) Neil Zimmermann (GSFC)

Future Plan and Facility

SPHERE+, Reaching New Depths

Anthony Boccaletti (LESIA, Observatoire de Paris), Absil O., Antoniucci S, Augereau J.-C., Baruffolo A, Baudino J.-L., Baudoz P., Beaulieu M., Benisty M., Beuzit J.-L., Bonnefoy M., Bos S., Brandner W., Cantalloube F., Carlotti A., Charnay B., Chauvin G., Choquet E., Claudi R., de Boer J., Desidera S., Delorme P., Doelman D., Dohlen K., Dominik C., DOrazi V., Engler N., Feldt M., Fusco T., Galicher R., Ghedina A., Ginski C., Gratadour D., Gratton R., Haffert S., Henning T., Houlle M., Huby E., Keller C., Kenworthy M., Kuhn J., Lagadec E., Lagrange A.-M., Langlois M., Le Coroller H., Li Causi G., Maire A.-L., Martinache F., Menard F., Mesa D., Meunier N., Milli J., Mouillet D., Mugnier L., NDiaye M, Otten G., Patapis P., Pedichini F., Por E., Potier A., Quanz S., Rouan D., Samland M., Sauvage J.-F., Schmid H.-M., Segransan D., Singh G., Snik F., Stangalini M., Tallon M., Turatto M., Udry S., Van Holstein R., Vigan A., Wildi F.

Exoplanet Sciences with Starshade

Renyu Hu (Jet Propulsion Laboratory, California Institute of Technology)

The game-changing promises of ELT/METIS for exoplanet imaging

Olivier Absil (University of Liege), Sascha Quanz (ETH Zurich)

REACH: Scientific Overview of Extremely High-Contrast Spectroscopy at the Subaru Telescope

Hajime Kawahara (The University of Tokyo), Takayuki Kotani (ABC), Masato Ishizuka (U.Tokyo), Olivier Guyon (Subaru, ABC, Arizona), Julien Lozi (Subaru), Nemanja Jovanovic (Caltech), Sebastien Vievard (Subaru, ABC, LESIA), Ananya Sahoo (Subaru)

High Contrast Imaging of Exoplanets and Exoplanetary Systems with JWST

Sasha Hinkley (University of Exeter), Aarynn Carter (Exeter), Andrew Skemer (UCSC), Beth Biller (Edinburgh), and 120 other collaborators.

Searching and characterizing exoplanetary gems with ECLIPS, the LUVOIR coronagraph instrument.

88 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Laurent A. Pueyo (STScI), and LUVOIR team (full list of authors will be provided at a later time it keeps being tweaked).

Exoplanet direct detection and characterization with the ELT/HARMONI integral field spectrograph

Mathis Houlle (Laboratoire d'Astrophysique de Marseille (LAM)), Arthur Vigan (Laboratoire d'Astrophysique de Marseille), Alexis Carlotti (Institut de Planetologie et d'Astrophysique de Grenoble), Elodie Choquet (Laboratoire d'Astrophysique de Marseille), Mickael Bonnefoy (Institut de Planetologie et d'Astrophysique de Grenoble), Niranjan Thatte (Department of Physics, University of Oxford), and Benoit Neichel (Laboratoire d'Astrophysique de Marseille)

The NASA/NSF Extreme Precision Radial Velocity Initiative

Karl Stapelfeldt (Jet Propulsion Laboratory, California Institute of Technology), Scott Gaudi (Ohio State), Gary Blackwood, Jennifer Burt, Eric Mamajek (JPL/Caltech), Chas Beichman (NExScI/Caltech), Heather Cegla (Geneva), Debra Fischer (Yale), Eric Ford (Penn State), Andrew Howard (Caltech), David Latham (Harvard CfA), Peter Plavchan (George Mason Univ.), and Andreas Quirrenbach (Landessternwarte Heidelberg)

The NASA Exoplanet Exploration Program Science Gap List

Karl Stapelfeldt (Jet Propulsion Laboratory, California Institute of Technology), Eric Mamajek (JPL/Caltech)

Directly Imaging Exoplanets and Disks with JWST NIRCam

Jarron Leisenring (University of Arizona), NIRCam Science GTO Team

A Standard comparison of exoplanet yield for the LUVOIR and HabEx Concept Studies

Rhonda Morgan (NASA/JPL), Standards Development and Evaluation Team: Dmitry Savransky (Cornell), Chris Stark(STScI), Eric Nielsen (Stanford), Bertrand Mennesson(JPL), Rus Belikov (Ames); Michael Turmon (JPL), Walker Dula (JPL), Gabriel Soto (Cornell), Dean Keithly (Cornell), Dan Sirbu (Ames), Peter Plavchan (George Mason), Shannon Dulz (Notre Dame)

Planet formation and Exoplanets at the Era of the Extremely Large Telescope

Gael Chauvin (International Franco-Chilean Laboratory for Astronomy,), ESO PST Team

High Contrast Observations with the Habitable Exoplanet Observatory (HabEx): Science Goals and Projected Capabilities

Bertrand Mennesson (Jet Propulsion Laboratory), S.Seager, K. Warfield, A. Kiessling, S. Martin, G. Kuan and the HabEx Study Team

Exoplanet Imaging with the Planetary Systems Imager

89 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Rebecca Jensen-Clem (UC Berkeley Astronomy Department), Michael Fitzgerald (UCLA), Mark Chun (UH), Olivier Guyon (Subaru), Nemanja Jovanovic (Caltech), Bruce Macintosh (Stanford), Dimitri Mawet (Caltech), Benjamin Mazin (UCSB), Andrew Skemer (UCSC), and the PSI Team

An Overview of the TMT Planetary Systems Imager

Michael Fitzgerald (Infrared Laboratory)

Others

Chasing free-floating planet from a parallax observation of a microlensing event

Makiko Ban (National Astronomical Observatory of Japan)

High contrast shock emission structures around VV CrA in datacube data achieved by high spectral resolution (R ~45000)

Tae-Soo Pyo (Subaru Telescope/NAOJ), Heeyoung Oh (KASI), In-Soo Yuk (KASI)

Vegetation red edge on water planets around M-dwarfs

Kenji Takizawa (Astrobiology Center)

90 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

91 In the Spirit of Lyot 2019, Tokyo, Japan, Oct. 21-25, 2019

Map (Plaza Heisei)

1st Floor

to 3rd floor

Posters

3rd Floor

Posters

Main session

92